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3036619

https://en.wikipedia.org/wiki/825%20Tanina

825 Tanina

825 Tanina (prov. designation: or ) is a stony background asteroid from the region of the Flora family, located in the inner part of the asteroid belt. It was discovered on 27 March 1916, by Russian astronomer Grigory Neujmin at the Simeiz Observatory on Crimea. The elongated S-type asteroid (SR) has a rotation period of 6.9 hours and measures approximately in diameter. Any reference of the asteroid's name to a person is unknown. Orbit and classification Tanina is a non-family asteroid of the main belt's background population when applying the hierarchical clustering method (HCM) by Nesvorný to its proper orbital elements. In the 1995 HCM-analysis by Zappalà, however, Tanina is a member of the Flora family (), a giant asteroid family and the largest family of stony asteroids in the main-belt. In the HCM-analysis by Milani and Knežević (AstDys), it is also a background asteroid as this analysis does not recognize the Flora asteroid clan. The asteroid orbits the Sun in the inner main-belt at a distance of 2.1–2.4 AU once every 3 years and 4 months (1,213 days; semi-major axis of 2.23 AU). Its orbit has an eccentricity of 0.08 and an inclination of 3° with respect to the ecliptic. Discovery Tanina was discovered by Russian astronomer Grigory Neujmin at the Simeiz Observatory on Crimean peninsula on 27 March 1916. One week later, on 3 April 1916, it was independently discovered by Max Wolf at the Heidelberg Observatory in Germany. The Minor Planet Center only recognizes the first discoverer. The asteroid was first observed as at Heidelberg on 17 October 1904, while the body's observation arc begins with Wolf's independent discovery observation. Naming This minor planet was named "Tanina". Any reference of its name to a person or occurrence is unknown. Unknown meaning Among the many thousands of named minor planets, Tanina is one of 120 asteroids for which has been published. All of these asteroids have low numbers, the first one being . The last asteroid with a name of unknown meaning is . They were discovered between 1876 and the 1930s, predominantly by astronomers Auguste Charlois, Johann Palisa, Max Wolf and Karl Reinmuth. Physical characteristics In the Tholen classification, Tanina is closest to a stony S-type asteroid, and somewhat similar to an uncommon R-type asteroid, while in the SMASS classification by Bus–Binzel, Tanina is a common S-type asteroid. Rotation period In February 2002, a rotational lightcurve of Tanina was obtained from photometric observations by Italian astronomer Andrea Ferrero at the Bigmuskie Observatory . Lightcurve analysis gave a well-defined rotation period of hours with a high brightness variation of magnitude, indicative of an elongated, non-spherical shape (). The result supersedes previous period determinations of hours with an amplitude of magnitude () by Wiesław Z. Wiśniewski from February 1992, and hours with an amplitude of magnitude () by Agnieszka Kryszczyńska in May 1999. In 2011, a modeled lightcurve using data from the Uppsala Asteroid Photometric Catalogue (UAPC) and other sources gave a sidereal period hours, as well as two spin axes at (46.0°, 48.0°) and (231.0°, 60.0°) in ecliptic coordinates (λ, β). Diameter and albedo According to the surveys carried out by the Infrared Astronomical Satellite IRAS, and the Japanese Akari satellite, and the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer (WISE), Tanina measures (), () and () kilometers in diameter and its surface has an albedo of (), () and (), respectively. The Collaborative Asteroid Lightcurve Link adopts an albedo of 0.1508 from Petr Pravec's revised WISE data, and takes a diameter of 14.67 kilometers based on an absolute magnitude of 11.84. Alternative mean-diameter measurements published by the WISE team include () and () with corresponding albedos of () and (). References External links Lightcurve Database Query (LCDB), at www.minorplanet.info Dictionary of Minor Planet Names, Google books Asteroids and comets rotation curves, CdR – Geneva Observatory, Raoul Behrend Discovery Circumstances: Numbered Minor Planets (1)-(5000) – Minor Planet Center 000825 Discoveries by Grigory Neujmin Named minor planets 000825 000825 19160327

3036624

https://en.wikipedia.org/wiki/826%20Henrika

826 Henrika

826 Henrika (prov. designation: or ) is a background asteroid from the central regions of the asteroid belt. It was discovered by German astronomer Max Wolf at the Heidelberg-Königstuhl State Observatory on 28 April 1916. The carbonaceous C-type asteroid has a rotation period of 5.98 hours and measures approximately in diameter. Any reference to the origin of the asteroid's name is unknown. Orbit and classification Henrika is a non-family asteroid of the main belt's background population when applying the hierarchical clustering method to its proper orbital elements. It orbits the Sun in the central asteroid belt at a distance of 2.2–3.3 AU once every 4 years and 6 months (1,631 days; semi-major axis of 2.71 AU). Its orbit has an eccentricity of 0.21 and an inclination of 7° with respect to the ecliptic. The body's observation arc begins at Heidelberg Observatory on 2 July 1921, more than five years after its official discovery observation. Naming Any reference of this minor planet name to a person or occurrence is unknown. Unknown meaning Among the many thousands of named minor planets, Henrika is one of 120 asteroids for which has been published. All of these asteroids have low numbers, the first one being . The last asteroid with a name of unknown meaning is . They were discovered between 1876 and the 1930s, predominantly by astronomers Auguste Charlois, Johann Palisa, Max Wolf and Karl Reinmuth. Physical characteristics In the Bus–Binzel SMASS classification, Henrika is a common, carbonaceous C-type asteroid, with an untypically high albedo (see below) for such spectral class. In a taxonomic classification based on MOVIS near-infrared colors, Henrika could not be assigned a final class and was labelled as undefined (U). Rotation period In April 210, a rotational lightcurve of Henrika was obtained from six nights of photometric observations by Frederick Pilcher at the Organ Mesa Observatory in New Mexico. Analysis of the classically shaped bimodal lightcurve gave a well-defined rotation period of hours with a brightness variation of magnitude (). During the same apparition, a virtually identical period of hours with an amplitude of magnitude () was determined by Kenda Albers and colleges of the Rose-Hulman Institute of Technology at the Oakley Southern Sky Observatory in Australia. Diameter and albedo According to the surveys carried out by the Infrared Astronomical Satellite IRAS, and the Japanese Akari satellite, and the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer (WISE), Henrika measures (), () and () kilometers in diameter and its surface has an albedo of (), () and (), respectively. Alternative mean-diameters published by the WISE team include (), () and () with corresponding albedos of (), () and (). The Collaborative Asteroid Lightcurve Link derives an albedo of 0.1103 and a diameter of 19.15 kilometers based on an absolute magnitude of 11.6. An asteroid occultations of Henrika from 19 January 2010, gave a best-fit ellipse dimension of (). These timed observations are taken when the asteroid passes in front of a distant star. Notes References External links Lightcurve Database Query (LCDB), at www.minorplanet.info Dictionary of Minor Planet Names, Google books Discovery Circumstances: Numbered Minor Planets (1)-(5000) – Minor Planet Center 000826 Discoveries by Max Wolf Named minor planets 000826 19160428

3036625

https://en.wikipedia.org/wiki/827%20Wolfiana

827 Wolfiana

827 Wolfiana, provisional designation , is a Florian asteroid from the inner regions of the asteroid belt, approximately 8 kilometers in diameter. It was discovered at Vienna Observatory on 29 August 1916, by Austrian astronomer Johann Palisa, who named it after German astronomer Max Wolf. The assumed stony asteroid has a rotation period of 4.0654 hours. Orbit and classification Wolfiana is a member of the Flora family (), a giant asteroid family and the largest family of stony asteroids in the main belt. It orbits the Sun in the inner asteroid belt at a distance of 1.9–2.6 AU once every 3 years and 5 months (1,253 days; semi-major axis of 2.27 AU). Its orbit has an eccentricity of 0.16 and an inclination of 3° with respect to the ecliptic. The body's observation arc begins with its official discovery observation at Vienna. Physical characteristics Wolfiana is an assumed stony S-type asteroid, which agrees with the overall spectral type for Florian asteroids. Rotation period In September 2012, a rotational lightcurve of Wolfiana was obtained from photometric observations by American astronomers Luis Martinez, Arizona, and Frederick Pilcher at Organ Mesa Observatory (), New Mexico. Lightcurve analysis gave a well-defined rotation period of 4.0654 hours with a brightness amplitude of 0.20 magnitude (), refining a period of 4.0 hours previously measured in November 2009 (). Diameter and albedo According to the survey carried out by the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer, Wolfiana measures 8.488 and 8.976 kilometers in diameter and its surface has an albedo of 0.129 and 0.1153, respectively. The Collaborative Asteroid Lightcurve Link assumes a standard albedo of 0.24 – derived from 8 Flora, the parent body of the Flora family – and calculates a diameter of 6.51 kilometers based on an absolute magnitude of 13.1. Naming This minor planet was named by the discoverer in 1920 () after German astronomer, colleague and friend, Max Wolf (1863–1932), a professor of astronomy at Heidelberg University and founder and director of the Heidelberg-Königstuhl State Observatory, who discovered several novae, comets and 248 minor planets. The official naming citation was mentioned in The Names of the Minor Planets by Paul Herget in 1955 (). Asteroid 1217 Maximiliana and the lunar crater Wolf were also named in his honor. References External links Asteroid Lightcurve Database (LCDB), query form (info ) Dictionary of Minor Planet Names, Google books Asteroids and comets rotation curves, CdR – Observatoire de Genève, Raoul Behrend Discovery Circumstances: Numbered Minor Planets (1)-(5000) – Minor Planet Center 000827 Discoveries by Johann Palisa Named minor planets 19160829

3036628

https://en.wikipedia.org/wiki/828%20Lindemannia

828 Lindemannia

828 Lindemannia is a minor planet orbiting the Sun with an orbital period of five years and 255 days. It was discovered on 29 August 1916 at the University of Vienna by Johann Palisa. It is named after Adolph Friedrich Lindemann, a British astronomer, engineer and businessman. See also List of asteroids/1–1000 References External links 000828 Discoveries by Johann Palisa Named minor planets 000828 19160829

3036630

https://en.wikipedia.org/wiki/830%20Petropolitana

830 Petropolitana

830 Petropolitana (prov. designation: or ) is a bright background asteroid from the outer regions of the asteroid belt. It was discovered on 25 August 1916, by Russian astronomer Grigory Neujmin at the Simeiz Observatory on the Crimean peninsula. The stony S-type asteroid has a long rotation period of 39.0 hours and measures approximately in diameter. It was named after the Russian city of Saint Petersburg. Orbit and classification Petropolitana is a non-family asteroid of the main belt's background population when applying the hierarchical clustering method to its proper orbital elements. It orbits the Sun in the outer asteroid belt at a distance of 3.0–3.4 AU once every 5 years and 9 months (2,099 days; semi-major axis of 3.21 AU). Its orbit has an eccentricity of 0.06 and an inclination of 4° with respect to the ecliptic. The body's observation arc begins at Heidelberg Observatory on 3 September 1916, or nine nights after its official discovery observation at Simeiz. Naming This minor planet was named by its Latin name "Petropolis", after the Russian city of Saint Petersburg. On the same night, Grigory Neujmin also discovered 829 Academia. Both asteroid were named on the occasion of the 200th anniversary of the founding of the Academy of Sciences in Staint Petersburg. The was also mentioned in The Names of the Minor Planets by Paul Herget in 1955 (). Physical characteristics In the Tholen classification, Petropolitana is a stony S-type asteroid, which are more common in the inner than in the outer asteroid belt. Rotation period In March 2005, a rotational lightcurve of Petropolitana was obtained from photometric observations by French amateur astronomer Pierre Antonini. Lightcurve analysis gave a rotation period of hours with a brightness variation of magnitude (). In 2016, a modeled lightcurve gave a concurring sidereal period of hours using data from a large collaboration of individual observers (such as above). The study also determined two spin axes of (217.0°, 36.0°) and (34.0°, 41.0°) in ecliptic coordinates (λ, β). In 2018, however, an international photometric survey, using archived photometric data from the Geneva Observatory as well from dedicated observations, modeled a far longer period of hours with an amplitude of magnitude (). The survey uses combines convex lightcurve inversion with a non-convex algorithm (SAGE) to derive their periods. Diameter and albedo According to the surveys carried out by the Infrared Astronomical Satellite IRAS, the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer (WISE), and the Japanese Akari satellite, Petropolitana measures (), () and () kilometers in diameter and its surface has an albedo of (), () and (), respectively. Alternative mean-diameters published by the WISE team include () and () with corresponding albedos of () and (). The Collaborative Asteroid Lightcurve Link, adopts the results obtained by IRAS, that is an albedo of 0.2382 and a diameter of 41.22 kilometers based on an absolute magnitude of 9.10. Two asteroid occultations of Petropolitana from May 2012 and September 2015, gave a best-fit ellipse dimension of () and (), respectively. These timed observations are taken when the asteroid passes in front of a distant star. References External links Lightcurve Database Query (LCDB), at www.minorplanet.info Dictionary of Minor Planet Names, Google books Asteroids and comets rotation curves, CdR – Geneva Observatory, Raoul Behrend Discovery Circumstances: Numbered Minor Planets (1)-(5000) – Minor Planet Center 000830 Discoveries by Grigory Neujmin Named minor planets 000830 19160825

3036634

https://en.wikipedia.org/wiki/831%20Stateira

831 Stateira

831 Stateira is an asteroid belonging to the Baptistina family in the Main Belt named after Stateira, wife of Artaxerexes II. References External links 000831 Discoveries by Max Wolf Named minor planets 19160920

3036639

https://en.wikipedia.org/wiki/834%20Burnhamia

834 Burnhamia

834 Burnhamia (prov. designation: or ) is a large background asteroid, approximately in diameter, that is located in the outer region of the asteroid belt. It was discovered on 20 September 1916, by German astronomer Max Wolf at the Heidelberg Observatory in southwest Germany. The X-type asteroid (GS) has a rotation period of 13.9 hours. It was named after American astronomer Sherburne Wesley Burnham (1838–1921). Orbit and classification Burnhamia is a non-family asteroid of the main belt's background population when applying the hierarchical clustering method to its proper orbital elements. It orbits the Sun in the outer main-belt at a distance of 2.5–3.8 AU once every 5 years and 8 months (2,076 days; semi-major axis of 3.18 AU). Its orbit has an eccentricity of 0.20 and an inclination of 4° with respect to the ecliptic. The asteroid's observation arc begins with its first observation as at Heidelberg Observatory on 26 October 1905, almost 11 years prior to its official discovery observation. Naming This minor planet was named after Sherburne Wesley Burnham (1838–1921), American astronomer who discovered many visual binary stars and is known for his Burnham Double Star Catalogue (BDS), a catalogue of double stars seen in the Northern Hemisphere, which was published in two parts by the Carnegie Institution of Washington in 1906. Burnham observed from the Chicago (1877), Lick (1888) and Yerkes (1897) observatories. The was published in the journal Astronomische Nachrichten in 1921 (), and was also mentioned in The Names of the Minor Planets by Paul Herget in 1955 (). The lunar crater Burnham is also named in his honor. Physical characteristics In the Tholen classification, Burnhamia is closest to a G-type asteroid and somewhat similar to a common stony S-type asteroid, while In ioth the Tholen- and SMASS-like taxonomy of the Small Solar System Objects Spectroscopic Survey (S3OS2), Burnhamia is an X-type asteroid. Rotation period In October 2006, a rotational lightcurve of Burnhamia was obtained from photometric observations by Robert Buchheim at the Altimira Observatory in California. Lightcurve analysis gave a well-defined rotation period of hours with a brightness variation of magnitude (). The result supersedes previous observations by French amateur astronomer Laurent Bernasconi from May 2005, with a period of hours with an amplitude of magnitude (), and from October 2006, that gave a period of hours and an amplitude of magnitude (). Diameter and albedo According to the surveys carried out by the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer (WISE), the Japanese Akari satellite, and the Infrared Astronomical Satellite IRAS, Burnhamia measures (), () and () kilometers in diameter and its surface has an albedo of (), () and (), respectively. The Collaborative Asteroid Lightcurve Link derives an albedo of 0.0602 and a diameter of 66.64 kilometers based on an absolute magnitude of 9.55. The WISE team also published an alternative mean-diameter of () with corresponding albedos of (). Two asteroid occultations of Burnhamia September 2013 and January 2014, gave both a best-fit ellipse dimension of (). These timed observations are taken when the asteroid passes in front of a distant star. References External links Lightcurve Database Query (LCDB), at www.minorplanet.info Dictionary of Minor Planet Names, Google books Asteroids and comets rotation curves, CdR – Geneva Observatory, Raoul Behrend Discovery Circumstances: Numbered Minor Planets (1)-(5000) – Minor Planet Center 000834 Discoveries by Max Wolf Named minor planets 000834 19160920

3036640

https://en.wikipedia.org/wiki/832%20Karin

832 Karin

832 Karin is a minor planet orbiting the Sun. It is the largest and brightest member of the Karin Cluster, which is named after it. Found in 2002, the Karin cluster is notable for being very young. It is currently believed to have formed in a collision only 5.8 million years ago. 832 Karin is an S-Type asteroid, approximately 19 km in diameter. The minor planet is named in honor of Karin Månsdotter, who was the mistress of Erik XIV of Sweden in the 16th century. In 1567, Erik married Karin, but he was pushed from his throne because of this marriage. References External links Asteroid Lightcurve Database (LCDB), query form (info ) Discovery Circumstances: Numbered Minor Planets (1)–(5000) Minor Planet Center 000832 000832 Discoveries by Max Wolf Named minor planets 19160920

3036642

https://en.wikipedia.org/wiki/833%20Monica

833 Monica

833 Monica is a minor planet orbiting the Sun. Measurements of the lightcurve made in 2010 give a rotation period of 12.09 ± 0.01 hours. It has a diameter of 21.2 km. References External links 000833 Discoveries by Max Wolf Named minor planets 19160920

3036645

https://en.wikipedia.org/wiki/835%20Olivia

835 Olivia

835 Olivia (prov. designation: or ) is a dark background asteroid from the outer regions of the asteroid belt. It was discovered by German astronomer Max Wolf at the Heidelberg-Königstuhl State Observatory on 23 September 1916. The carbonaceous C-type asteroid measures approximately in diameter, and is one of few low-numbered asteroids with an undetermined rotation period. Any reference to the origin of the asteroid's name is unknown. Orbit and classification Olivia is a non-family asteroid of the main belt's background population when applying the hierarchical clustering method to its proper orbital elements. It orbits the Sun in the outer asteroid belt at a distance of 2.9–3.5 AU once every 5 years and 9 months (2,109 days; semi-major axis of 3.22 AU). Its orbit has an eccentricity of 0.09 and an inclination of 4° with respect to the ecliptic. The body's observation arc begins at the Bergedorf Observatory on 30 September 1916, one week after its official discovery observation at Heidelberg. Naming Any reference of this minor planet name to a person or occurrence is unknown. Unknown meaning Among the many thousands of named asteroids, Olivia is one of 120 planets for which has been published. All of these asteroids have low numbers, the first one being . The last asteroid with a name of unknown meaning is . They were discovered between 1876 and the 1930s, predominantly by astronomers Auguste Charlois, Johann Palisa, Max Wolf and Karl Reinmuth. Physical characteristics In the SDSS-based taxonomy, Olivia is a common, carbonaceous C-type asteroid, with a notably low albedo (see below). Rotation period As of 2020, no rotational lightcurve of Olivia has been obtained from photometric observations. The body's rotation period, pole and shape remain unknown. Diameter and albedo According to the surveys carried out by the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer (WISE), the Infrared Astronomical Satellite IRAS, and the Japanese Akari satellite, Olivia measures (), () and () kilometers in diameter and its surface has a notably low albedo of (), () and (), respectively. Alternative mean-diameters published by the WISE team include () and () with corresponding albedos of () and (). References External links Lightcurve Database Query (LCDB), at www.minorplanet.info Dictionary of Minor Planet Names, Google books Discovery Circumstances: Numbered Minor Planets (1)-(5000) – Minor Planet Center 000835 Discoveries by Max Wolf Named minor planets 19160923

3036651

https://en.wikipedia.org/wiki/836%20Jole

836 Jole

836 Jole (prov. designation: or ) is a bright background asteroid from the inner regions of the asteroid belt. It was discovered on 23 September 1916, by German astronomer Max Wolf at the Heidelberg Observatory in southwest Germany. The stony S-type asteroid has a rotation period of 9.6 hours and measures approximately in diameter. It was named after Iole, wife of Heracles from Greek mythology. Orbit and classification Located in the orbital region of the Flora family, Jole is a non-family asteroid of the main belt's background population when applying the hierarchical clustering method to its proper orbital elements. It orbits the Sun in the inner asteroid belt at a distance of 1.8–2.6 AU once every 3 years and 3 months (1,184 days; semi-major axis of 2.19 AU). Its orbit has an eccentricity of 0.18 and an inclination of 5° with respect to the ecliptic. The asteroid was first observed as A903 QA at Heidelberg Observatory on 24 August 1903, where the body's observation arc begins on the following night. Naming Based on Lutz Schmadel's own research, this minor planet was named from Greek mythology, after Iole, daughter of King Eurytus of Oechalia and wife by force of divine hero Heracles. The naming was not mentioned in The Names of the Minor Planets by Paul Herget in 1955. Physical characteristics In the SDSS-based taxonomy, Jole is a common, stony S-type asteroid. Rotation period In September 2010, a rotational lightcurve of Jole was obtained from photometric observations by Daniel Coley at the DanHenge Observatory at the Center for Solar System Studies. Lightcurve analysis gave a well-defined rotation period of hours with a brightness variation of magnitude (). Diameter and albedo According to the survey carried out by the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer (WISE), Jole measures kilometers in diameter and its surface has an albedo of . Alternative mean-diameters published by the WISE team includes () and () with corresponding albedos of () and (). The Collaborative Asteroid Lightcurve Link assumes an albedo for a Florian asteroid of 0.24 and calculates a diameter of 6.21 kilometers based on an absolute magnitude of 13.2. Notes References External links Lightcurve Database Query (LCDB), at www.minorplanet.info Dictionary of Minor Planet Names, Google books Discovery Circumstances: Numbered Minor Planets (1)-(5000) – Minor Planet Center 000836 Discoveries by Max Wolf Named minor planets 19160923

3036653

https://en.wikipedia.org/wiki/837%20Schwarzschilda

837 Schwarzschilda

837 Schwarzschilda, provisional designation 1916 AG, is a low-eccentric, well-observed asteroid from the asteroid belt, orbiting the Sun with a period of 3.48 years at a distance of 2.21–2.39 AU. It was discovered by German astronomer Max Wolf at Heidelberg Observatory on 23 September 1916. The main-belt asteroid was named after physicist and astronomer Karl Schwarzschild (1873–1916), who had died earlier that year. He was director of the observatories in Göttingen and Potsdam, known for his work in photometry, geometrical optics, stellar statistics and theoretical astrophysics, most notably for producing the first exact solutions to Einstein's field equations. At the time, it was custom to give feminized names to minor planets. See also Meanings of minor planet names: 501–1000 Schwarzschild radius References External links Dictionary of Minor Planet Names, Google books 000837 Discoveries by Max Wolf Named minor planets 19160923

3036654

https://en.wikipedia.org/wiki/838%20Seraphina

838 Seraphina

838 Seraphina (prov. designation: or ) is a dark and large background asteroid, approximately in diameter, located in the outer regions of the asteroid belt. It was discovered by German astronomer Max Wolf at the Heidelberg-Königstuhl State Observatory on 24 September 1916. The primitive P-type asteroid has a rotation period of 15.7 hours and is rather spherical in shape. Any reference to the origin of the asteroid's name is unknown. Orbit and classification Seraphina is a non-family asteroid of the main belt's background population when applying the hierarchical clustering method to its proper orbital elements. It orbits the Sun in the outer asteroid belt at a distance of 2.5–3.3 AU once every 4 years and 11 months (1,802 days; semi-major axis of 2.9 AU). Its orbit has an eccentricity of 0.13 and an inclination of 10° with respect to the ecliptic. The body's observation arc begins with its official discovery observation at Heidelberg Observatory on 24 September 1916. Naming Any reference of this minor planet name to a person or occurrence is unknown. Unknown meaning Among the many thousands of named minor planets, Seraphina is one of 120 asteroids for which no official naming citation has been published. All of these asteroids have low numbers in between and and were discovered from 1876 up to the 1930s, predominantly by astronomers Auguste Charlois, Johann Palisa, Max Wolf and Karl Reinmuth. Physical characteristics In the Tholen classification, Seraphina is a very dark, primitive P-type asteroid, that falls into the wider group of the carbonaceous C-Complex. In both the Tholen- and SMASS-like taxonomy of the Small Solar System Objects Spectroscopic Survey (S3OS2), it is an X-type asteroid. P-type asteroids are common in the outer asteroid belt and among the Jupiter trojans. Rotation period In November 2005, a rotational lightcurve of Seraphina was obtained from photometric observations by French amateur astronomer Raymond Poncy. Lightcurve analysis gave a rotation period of hours with a low brightness variation of magnitude, indicative of a rather spherical shape (). Other observations include a period of hours with an amplitude of magnitude by Richard Binzel from June 1984 (), and a period of hours with an amplitude of magnitude by the Spanish group of asteroid observers, OBAS, in November 2015 (). In 2018, Czech astronomers Josef Ďurech and Josef Hanuš published a modeled lightcurve using photometric data from the Gaia spacecraft's second data release. It showed a sidereal period of hours (), and gave two spin axes at (18.0°, 4.0°) and (192.0°, 32.0°) in ecliptic coordinates (λ, β). Diameter and albedo According to the surveys carried out by the Japanese Akari satellite, the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer (WISE), and the Infrared Astronomical Satellite IRAS, Seraphina measures (), () and () kilometers in diameter and its surface has an albedo of (), () and (), respectively. The Collaborative Asteroid Lightcurve Link derives an albedo of 0.0427 and a diameter of 59.75 kilometers based on an absolute magnitude of 10.16. Alternative mean-diameter measurements published by the WISE team include (), () and () with corresponding albedos of (), () and (). Two asteroid occultations of Seraphina gave a best-fit ellipse dimension of () and () for their respective observation on 5 February 2007 and on 20 July 2014. These timed observations are taken when the asteroid passes in front of a distant star. However, these two observations have received a poor quality rating. References External links Lightcurve Database Query (LCDB), at www.minorplanet.info Dictionary of Minor Planet Names, Google books Asteroids and comets rotation curves, CdR – Geneva Observatory, Raoul Behrend Discovery Circumstances: Numbered Minor Planets (1)-(5000) – Minor Planet Center 000838 Discoveries by Max Wolf Named minor planets 000838 19160924

3036655

https://en.wikipedia.org/wiki/839%20Valborg

839 Valborg

839 Valborg is a mid-sized S-type Eunomian asteroid. Its diameter is about 20 km, its albedo of 0.353 is very high for an asteroid. Its rotation period is 10.366 hours. References External links Lightcurve plot of 839 Valborg, Palmer Divide Observatory, B. D. Warner (2005) Asteroid Lightcurve Database (LCDB), query form (info ) Dictionary of Minor Planet Names, Google books Asteroids and comets rotation curves, CdR – Observatoire de Genève, Raoul Behrend Discovery Circumstances: Numbered Minor Planets (1)-(5000) – Minor Planet Center 000839 Discoveries by Max Wolf Named minor planets 000839 19160924

3036659

https://en.wikipedia.org/wiki/840%20Zenobia

840 Zenobia

840 Zenobia is a minor planet orbiting the Sun. It was discovered by German astronomer Max Wolf at Heidelberg on September 25, 1916. The origin of the name is uncertain, but it may be named after the Slavic god of the hunt. Photometric observations of the asteroid during 2006 at the Palmer Divide Observatory in Colorado Springs, Colorado, were used to generate a light curve with a period of 5.565 ± 0.005 hours and a variation in brightness of 0.20 ± 0.02 magnitude. References External links Lightcurve plot of 840 Zenobia, Palmer Divide Observatory, B. D. Warner (2005) Asteroid Lightcurve Database (LCDB), query form (info ) Dictionary of Minor Planet Names, Google books Asteroids and comets rotation curves, CdR – Observatoire de Genève, Raoul Behrend Discovery Circumstances: Numbered Minor Planets (1)-(5000) – Minor Planet Center 000840 Discoveries by Max Wolf Named minor planets 19160925 Zenobia

3036663

https://en.wikipedia.org/wiki/841%20Arabella

841 Arabella

841 Arabella is an asteroid belonging to the Flora family in the Main Belt. Its rotation period is 3.39 hours. It is named after the title character from Richard Strauss' opera Arabella. References External links 000841 Discoveries by Max Wolf Named minor planets 19161001

3036664

https://en.wikipedia.org/wiki/842%20Kerstin

842 Kerstin

842 Kerstin (prov. designation: or ) is a dark background asteroid from the outer regions of the asteroid belt. It was discovered on 1 October 1916, by German astronomer Max Wolf at the Heidelberg-Königstuhl State Observatory in southwest Germany. The assumed C-type asteroid has a rotation period of 18.7 hours and measures approximately in diameter. Any reference of the origin of the asteroid's name is unknown. Orbit and classification Kerstin is a non-family asteroid of the main belt's background population when applying the hierarchical clustering method to its proper orbital elements. It orbits the Sun in the outer main-belt at a distance of 2.9–3.6 AU once every 5 years and 10 months (2,127 days; semi-major axis of 3.24 AU). Its orbit has an eccentricity of 0.12 and an inclination of 14° with respect to the ecliptic. The body's observation arc begins at Heidelberg Observatory with its official discovery observation on 1 October 1916. Naming "Kerstin" is a German feminine first name. Any reference of this name to a person or occurrence is unknown. Unknown meaning Among the many thousands of named minor planets, Kerstin is one of 120 asteroids for which no official naming citation has been published. All of these asteroids have low numbers between and and were discovered between 1876 and the 1930s, predominantly by astronomers Auguste Charlois, Johann Palisa, Max Wolf and Karl Reinmuth. Physical characteristics Kerstin is an assumed C-type asteroid, with a low astronomical albedo (see below) comparable to fresh asphalt. Rotation period In 2018, Czech astronomers Josef Ďurech and Josef Hanuš published a modeled lightcurve using photometric data from the Gaia spacecraft's second data release. It showed a sidereal period of hours (), and gave a spin axis at (18.0°, 78.0°) in ecliptic coordinates (λ, β). Diameter and albedo According to the surveys carried out by the Infrared Astronomical Satellite IRAS, the Japanese Akari satellite, and the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer (WISE), Kerstin measures (), () and () kilometers in diameter and its surface has an albedo of (), () and (), respectively. The Collaborative Asteroid Lightcurve Link assumes a standard albedo for a carbonaceous asteroid of 0.057 and calculates a diameter of 42.23 kilometers based on an absolute magnitude of 10.6. Alternative mean-diameter measurements published by the WISE team include (), (), () and () with corresponding albedos of (), (), () and (). References External links Lightcurve Database Query (LCDB), at www.minorplanet.info Dictionary of Minor Planet Names, Google books Asteroids and comets rotation curves, CdR – Geneva Observatory, Raoul Behrend Discovery Circumstances: Numbered Minor Planets (1)-(5000) – Minor Planet Center 000842 Discoveries by Max Wolf Named minor planets 19161001

3036665

https://en.wikipedia.org/wiki/843%20Nicolaia

843 Nicolaia

843 Nicolaia is a main-belt asteroid discovered by Danish astronomer H. Thiele on 30 September 1916. It was a lost asteroid for 65 years before being rediscovered by Astronomisches Rechen-Institut at Heidelberg in 1981. The asteroid is orbiting the Sun with a period of 3.44 years. References External links 000843 Discoveries by Holger Thiele Named minor planets 19160930

3036667

https://en.wikipedia.org/wiki/844%20Leontina

844 Leontina

844 Leontina, provisional designation 1916 AP, is a stony asteroid from the outer region of the asteroid belt, about 36 kilometers in diameter. It was discovered on 1 October 1916, by Austrian astronomer Joseph Rheden at Vienna Observatory, Austria. Description Leontina is an X-type asteroid in the SMASS classification. It orbits the Sun at a distance of 3.0–3.4 AU once every 5 years and 9 months (2,097 days). Its orbit is tilted by 9 degrees to the plane of the ecliptic and shows an eccentricity of 0.07. Multiple lightcurve analysis rendered a well-defined, concurring rotation period of 6.79 hours. According to the surveys carried out by the Japanese Akari satellite and the U.S. Wide-field Infrared Survey Explorer with its subsequent NEOWISE mission, measurements of the body's brightness gave a divergent albedo of 0.13, 0.20 and 0.31, respectively. As a result, the asteroid's estimated diameter strongly varies between 28 and 40 kilometers. The Collaborative Asteroid Lightcurve Link (CALL) considers Akari's albedo-figure of 0.20 the most accurate one and consequently assumes the otherwise classified X-type body to be of a stony surface composition with a calculated diameter of 36 kilometers. This minor planet was named by the discoverer for his home town Lienz in East Tyrol, Austria. References External links The Asteroid Veritas: An intruder in a family named after it? Asteroid Lightcurve Database (LCDB), query form (info ) Dictionary of Minor Planet Names, Google books Asteroids and comets rotation curves, CdR – Observatoire de Genève, Raoul Behrend Discovery Circumstances: Numbered Minor Planets (1)-(5000) – Minor Planet Center 000844 Discoveries by Joseph Rheden Named minor planets 000844 19161001

3036673

https://en.wikipedia.org/wiki/846%20Lipperta

846 Lipperta

846 Lipperta is a Themistian asteroid. Based on lightcurve studies, Lipperta has a rotation period of 1641 hours, but this figure is based on less than full coverage, so that the period may be wrong by 30 percent or so. The lack of variation in brightness could be caused by (a) very slow rotation, (b) near pole-on viewing aspect, or (c) a spherical body with uniform albedo. References External links 000846 Discoveries by K. Gyllenberg Named minor planets 000846 000846 19161126

3036675

https://en.wikipedia.org/wiki/847%20Agnia

847 Agnia

847 Agnia is a minor planet orbiting the Sun. It is approximately 28 kilometers in diameter. The spectrum of this object indicates that it is an S-type asteroid with both low and high calcium forms of pyroxene on the surface, along with less than 20% olivine. The high-calcium form of pyroxene forms 40% or more of the total pyroxene present, indicating a history of igneous rock deposits. This suggests that the asteroid underwent differentiation by melting, creating a surface of basalt rock. 847 Agnia is the namesake of the Agnia family of asteroids that share similar orbital elements and physical properties. The members of this family, including 847 Agnia, most likely formed from the breakup of a basalt object, which in turn was spawned from a larger parent body that had previously undergone igneous differentiation. Other members of this family include 1020 Arcadia, 1228 Scabiosa, 2401 Aehlita, and 3395 Jitka Photometric observations of this asteroid collected during 2004–2005 show a rotation period of 14.827 ± 0.001 hours with a brightness variation of 0.45 ± 0.03 magnitude. References External links Discovery Circumstances: Numbered Minor Planets 000847 Discoveries by Grigory Neujmin Named minor planets 000847 000847 19150902

3036676

https://en.wikipedia.org/wiki/848%20Inna

848 Inna

848 Inna (prov. designation: or ) is a carbonaceous Themistian asteroid from the outer regions of the asteroid belt. It was discovered on 5 September 1915, by astronomer Grigory Neujmin at the Simeiz Observatory on the Crimean peninsula. The C-type asteroid measures approximately in diameter, while its rotation period remains unknown. It was named after Russian astronomer Inna Nikolaevna Leman-Balanovskaya (1881–1945). Orbit and classification When applying the hierarchical clustering method to its proper orbital elements, Inna is a core member of the Themis family (), a very large family of carbonaceous asteroids, named after 24 Themis. It orbits the Sun in the outer main-belt at a distance of 2.6–3.6 AU once every 5 years and 6 months (2,003 days; semi-major axis of 3.11 AU). Its orbit has an eccentricity of 0.16 and an inclination of 1° with respect to the ecliptic. Discovery Inna was officially discovered on 5 September 1915, by Georgian–Russian astronomer Grigory Neujmin at the Simeiz Observatory on the Crimean peninsula. Four nights later, it was independently discovered by Max Wolf at Heidelberg Observatory on 9 September 1915, which is also the beginning of the body's observation arc. The Minor Planet Center, however, only credits the first astronomer with the discovery. The asteroid was first observed by Wolf as at Heidelberg on 27 December 1905. Naming This minor planet was named after Inna Nikolaevna Leman-Balanovskaya (1881–1945), a Russian astronomer at the Pulkovo Observatory near St Petersburg, Russia. The naming was not mentioned in The Names of the Minor Planets by Paul Herget in 1955. Lutz Schmadel, the author of the Dictionary of Minor Planet Names learned about the origin of the minor planet's name from private communications with astronomer Nikolai Chernykh (1931–2004), who worked as an astrometricist and Solar System dynamicist at the Crimean Astrophysical Observatory. Physical characteristics In the Tholen-like taxonomy of the Small Solar System Objects Spectroscopic Survey (S3OS2), Inna is a common carbonaceous C-type asteroid, while in the survey's SMASS-like taxonomic variant, it is a Cb-subtype, transitioning to the somewhat brighter B-type asteroids. The Themis family has a "CB" overall spectral type. , no rotational lightcurve of Inna has been obtained from photometric observations. The body's rotation period, pole and shape remain unknown. Diameter and albedo According to the survey carried out by the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer (WISE), Inna measures kilometers in diameter and its surface has an albedo of . Alternative mean-diameters published by the WISE team include () and () with corresponding albedos of () and (). References External links Lightcurve Database Query (LCDB), at www.minorplanet.info Dictionary of Minor Planet Names, Google books Asteroids and comets rotation curves, CdR – Geneva Observatory, Raoul Behrend Discovery Circumstances: Numbered Minor Planets (1)-(5000) – Minor Planet Center 000848 Discoveries by Grigory Neujmin Named minor planets 19150905

3036677

https://en.wikipedia.org/wiki/849%20Ara

849 Ara

849 Ara (prov. designation: or ) is a large, metallic background asteroid, approximately in diameter, that is located in the outer region of the asteroid belt. It was discovered on 9 February 1912, by Russian astronomer Sergey Belyavsky at the Simeiz Observatory on the Crimean peninsula. The M-type asteroid has a short rotation period of 4.1 hours and is likely elongated in shape. It was named after the American Relief Administration (ARA) for the help given during the Russian famine of 1921–22. Orbit and classification Ara is a non-family asteroid of the main belt's background population when applying the hierarchical clustering method to its proper orbital elements. It orbits the Sun in the outer asteroid belt at a distance of 2.5–3.8 AU once every 5 years and 7 months (2,038 days; semi-major axis of 3.15 AU). Its orbit has an eccentricity of 0.20 and an inclination of 20° with respect to the ecliptic. In addition, Ara has a low Jupiter tisserand of 3.09, just above the defined threshold of 3.0 which is used to distinguish asteroids from the Jupiter-family comets. The body's observation arc begins at the Collegio Romano Observatory in Italy on 3 July 1919, more than 6 years after its official discovery observation at Simeiz. Naming This minor planet was named after American Relief Administration (ARA), in appreciation of the help it gave during the Russian famine of 1921–22. Headed by Herbert Hoover, ARA was a relief mission after World War I to Europe which also included post-revolutionary Russia later on. The was mentioned in The Names of the Minor Planets by Paul Herget in 1955 (). Physical characteristics In the Tholen classification as well as in the lesser known taxonomic method by Howell, Ara is a metallic M-type asteroid. This spectral type translates into the X-type in more modern asteroid taxonomic systems. In 2018 and 2019, a study using photometry from the Korea Microlensing Telescope Network and the South African Astronomical Observatory, grouped Ara into the X-type category based on the Bus–DeMeo classification. Rotation period and pole In June 1981, a rotational lightcurve of Ara was obtained from photometric observations by Alan Harris. Lightcurve analysis gave a rotation period of hours with a brightness variation of magnitude, indicative of an elongated shape (). Numerous observations have since confirmed this period. This includes Laurent Bernasconi (2004) and (2006), Davide Gandolfi (2006), Adam Marciniak (2009), Maurice Audejean (2010), and Richard E. Schmidt (2017). In 2017, a modeled lightcurve gave a concurring sidereal period of hours as well as a spin axis of (223.0°, −41.0°) in ecliptic coordinates (λ, β). Diameter and albedo According to the surveys carried out by the Japanese Akari satellite, the Infrared Astronomical Satellite IRAS, and the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer (WISE), Ara measures (), () and () kilometers in diameter and its surface has an albedo of (), () and (), respectively. Alternative mean-diameters published by the WISE team include () and () with corresponding albedos of () and (). In 2009 and 2015, several asteroid occultations of Ara were observed. The two best-rated observations from January 2009 and April 2015 and August 2008, gave a best-fit ellipse dimension of () and (), respectively. These timed observations are taken when the asteroid passes in front of a distant star. The Collaborative Asteroid Lightcurve Link adopts Petr Pravec's revised WISE albedo of 0.1149 and takes a diameter of 84.61 kilometers based on an absolute magnitude of 8.33, while Josef Ďurech calculates a diameter of by combining lightcurve inversion models with asteroid occultation silhouettes. References External links Lightcurve Database Query (LCDB), at www.minorplanet.info Dictionary of Minor Planet Names, Google books Asteroids and comets rotation curves, CdR – Geneva Observatory, Raoul Behrend Discovery Circumstances: Numbered Minor Planets (1)-(5000) – Minor Planet Center 000849 Discoveries by Sergei Belyavsky Named minor planets 000849 19120209 vec:Lista de asteroidi#849 Ara

3036679

https://en.wikipedia.org/wiki/850%20Altona

850 Altona

850 Altona (prov. designation: or ) is a large background asteroid, approximately in diameter, that is located in the outer region of the asteroid belt. It was discovered on 27 March 1916, by Russian astronomer Sergey Belyavsky at the Simeiz Observatory on the Crimean peninsula. The X-type asteroid has a rotation period of 11.2 hours. It was named after the city of Altona near Hamburg, Germany. Orbit and classification Altona is a non-family asteroid of the main belt's background population when applying the hierarchical clustering method to its proper orbital elements. It orbits the Sun in the outer asteroid belt at a distance of 2.6–3.4 AU once every 5 years and 2 months (1,897 days; semi-major axis of 3 AU). Its orbit has an eccentricity of 0.13 and an inclination of 16° with respect to the ecliptic. The body's observation arc begins at Algiers Observatory in North Africa on 28 July 1917, more than a year after its official its discovery observation at the Simeiz Observatory on 27 March 1916. Naming This minor planet was named after Altona, Hamburg, the location of the Altona Observatory, at which Heinrich Christian Schumacher began publication of the astronomical journal Astronomische Nachrichten in 1821. Altona is the home-town of Friedrich Georg Wilhelm von Struve, who founded the Pulkovo Observatory near St Petersburg, Russia. The was also mentioned in The Names of the Minor Planets by Paul Herget in 1955 (). Physical characteristics In both the Tholen- and SMASS-like taxonomy of the Small Solar System Objects Spectroscopic Survey (S3OS2), Altona is an X-type asteroid. Rotation period In September 2017, a rotational lightcurve of Altona was obtained from photometric observations by Brian Warner at his Palmer Divide Station of the Center for Solar System Studies in California. Lightcurve analysis gave a well-defined rotation period of hours with a brightness variation of magnitude (). The result supersedes previous period determinations of: and hours by astronomers at the Palomar Transient Factory, California, in January 2014 (), hours by Michael Alkema at the Elephant Head Observatory in Arizona in December 2012 (), hours by Frederick Pilcher at the Organ Mesa Observatory in June 2010 (), and hours by Robin Esseiva, Nicolas Esseiva and Raoul Behrend in April 2015 (). Diameter and albedo According to the surveys carried out by the Japanese Akari satellite, the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer (WISE), and the Infrared Astronomical Satellite IRAS, Altona measures (), () and () kilometers in diameter and its surface has an albedo of (), () and (), respectively. The Collaborative Asteroid Lightcurve Link derives an albedo of 0.0356 and a diameter of 80.85 kilometers based on an absolute magnitude of 9.7. Alternative mean-diameter measurements published by the WISE team include (), (), () and () with corresponding albedos of (), (), (), and (). An asteroid occultation observed on 3 April 2008, gave a best-fit ellipse dimension of (). These timed observations are taken when the asteroid passes in front of a distant star. Notes References External links Lightcurve Database Query (LCDB), at www.minorplanet.info Dictionary of Minor Planet Names, Google books Asteroids and comets rotation curves, CdR – Geneva Observatory, Raoul Behrend Discovery Circumstances: Numbered Minor Planets (1)-(5000) – Minor Planet Center 000850 Discoveries by Sergei Belyavsky Named minor planets 19160327

3036683

https://en.wikipedia.org/wiki/851%20Zeissia

851 Zeissia

851 Zeissia is an S-type asteroid background asteroid from the inner region of the asteroid belt. Its diameter is about 12 km and it has an albedo of 0.2646 . Its rotation period is 9.34 hours. The asteroid is named after the German optician and company founder Carl Zeiss. References External links 000851 Discoveries by Sergei Belyavsky Named minor planets 000851 19160402

3036684

https://en.wikipedia.org/wiki/852%20Wladilena

852 Wladilena

852 Wladilena is a Phocaea asteroid from the inner region of the asteroid belt. It is named after the Russian Communist leader Vladimir Lenin. References External links 000852 Discoveries by Sergei Belyavsky Named minor planets 19160402

3036685

https://en.wikipedia.org/wiki/853%20Nansenia

853 Nansenia

853 Nansenia is a minor planet orbiting the Sun. It is named after the Norwegian polar explorer and Nobel Peace Prize laureate Fridtjof Nansen. References External links 000853 Discoveries by Sergei Belyavsky Named minor planets 000853 000853 19160402 Fridtjof Nansen

3036687

https://en.wikipedia.org/wiki/854%20Frostia

854 Frostia

854 Frostia is a main-belt asteroid orbiting the Sun. It was discovered in 1916 by Sergei Ivanovich Belyavsky from Simeiz Observatory in Crimea and is named after Edwin Brant Frost, an American astronomer. This asteroid measures approximately in diameter. A satellite, designated S/2004 (854) 1, was identified based on light curve observations in July 2004 by Raoul Behrend, Laurent Bernasconi, Alain Klotz, and Russell I. Durkee. It is roughly in diameter and orbits about from Frostia with an orbital period of 1.572 days. References External links Discovery Circumstances: Numbered Minor Planets (1)-(5000) – Minor Planet Center (854) Frostia, datasheet, johnstonsarchive.net Asteroids with Satellites, Robert Johnston, johnstonsarchive.net IAUC 8389 announcing the satellite 000854 Discoveries by Sergei Belyavsky Named minor planets 000854 19160403 20040717

3036691

https://en.wikipedia.org/wiki/855%20Newcombia

855 Newcombia

855 Newcombia (prov. designation: or ) is a stony background asteroid from the inner regions of the asteroid belt. It was discovered on 3 April 1916, by astronomer Sergey Belyavsky at the Simeiz Observatory on the Crimean peninsula. The S-type asteroid has a notably short rotation period of 3.0 hours and measures approximately in diameter. It was named after Canadian–American astronomer Simon Newcomb (1835–1909). Orbit and classification Newcombia is a non-family asteroid of the main belt's background population when applying the hierarchical clustering method to its proper orbital elements. It orbits the Sun in the inner main-belt at a distance of 1.9–2.8 AU once every 3 years and 8 months (1,326 days; semi-major axis of 2.36 AU). Its orbit has an eccentricity of 0.18 and an inclination of 11° with respect to the ecliptic. Discovery Newcombia was discovered by Soviet-Russian astronomer Sergey Belyavsky at the Simeiz Observatory on the Crimean peninsula on 3 April 1916. The body's observation arc begins three weeks later, with its independent discovery by Max Wolf at Heidelberg Observatory on 28 April 2016. The Minor Planet Center, however, only credits the first discoverer. Naming This minor planet was named after Simon Newcomb (1835–1909), a Canadian–American professor of astronomy and director of the U.S. Nautical Almanac Office at the United States Naval Observatory. He worked on cometary and planetary orbits and is known for his Tables of the Motion of the Earth on its Axis and Around the Sun, a mathematical development of the position of the Earth in the Solar System. Newcomb also measured the speed of light and revised the astronomical unit. The was mentioned in The Names of the Minor Planets by Paul Herget in 1955 (). The lunar crater Newcomb as well as the Martian crater Newcomb were also named in his honor. Physical characteristics In the SDSS-based taxonomy, Newcombia is a common, stony S-type asteroid. Rotation period In October 2004, a rotational lightcurve of Newcombia was obtained from photometric observations by American amateur astronomer Walter R. Cooney Jr. in collaboration with John Gross, Dirk Terrell, Vishnu Reddy and Ron Dyvig. Lightcurve analysis gave a well-defined rotation period of hours with a brightness variation of magnitude (). An identical period of hours with an amplitude of magnitude was determined in April 2014, by Daniel Klinglesmith and colleagues at the Etscorn Observatory in New Mexico (). Klinglesmith also published a period of in November 2015 and January 2017 (). Two more lightcurves by Robert Stephens at the Center for Solar System Studies gave a period of and hours with a brightness variation of and magnitude in March 2014 and September 2019, respectively (). Diameter and albedo According to the surveys carried out by the Japanese Akari satellite and the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer (WISE), Newcombia measures () and () kilometers in diameter and its surface has an albedo of () and (), respectively. The Collaborative Asteroid Lightcurve Link assumes a standard albedo for a stony asteroid of 0.20 and calculates a diameter of 13.58 kilometers based on an absolute magnitude of 11.7. Alternative mean-diameter measurements published by the WISE team include () and () with corresponding albedos of () and (). Notes References External links Lightcurve Database Query (LCDB), at www.minorplanet.info Dictionary of Minor Planet Names, Google books Asteroids and comets rotation curves, CdR – Geneva Observatory, Raoul Behrend Discovery Circumstances: Numbered Minor Planets (1)-(5000) – Minor Planet Center 000855 Discoveries by Sergei Belyavsky Named minor planets 19160403 Ceres trojans

3036693

https://en.wikipedia.org/wiki/856%20Backlunda

856 Backlunda

856 Backlunda (prov. designation: or ) is a dark background asteroid from the inner region of the asteroid belt. It was discovered on 3 April 1916, by Russian astronomer Sergey Belyavsky at the Simeiz Observatory on the Crimean peninsula. The carbonaceous C-type asteroid has a rotation period of 12.1 hours and measures approximately in diameter. It was named after Swedish-Russian astronomer Oskar Backlund (1846–1916). Orbit and classification Backlunda is a non-family asteroid of the main belt's background population when applying the hierarchical clustering method to its proper orbital elements. It orbits the Sun in the inner asteroid belt at a distance of 2.1–2.7 AU once every 3 years and 10 months (1,388 days; semi-major axis of 2.43 AU). Its orbit has an eccentricity of 0.12 and an inclination of 14° with respect to the ecliptic. The asteroid was first observed as at Taunton Observatory in February 1908. The body's observation arc begins at Algiers Observatory in North Africa on 28 February 1931, almost 15 years after to its official discovery observation at Simeiz. Naming This minor planet was named after Swedish-born Russian astronomer Oskar Backlund (1846–1916), who is known for studying the orbit of comets, in particular that of Comet Encke. The was mentioned in The Names of the Minor Planets by Paul Herget in 1955 (). The astronomer is also honored by the 75-kilometer lunar crater Backlund. Physical characteristics In the Bus–Binzel SMASS classification, Backlunda is a common carbonaceous C-type asteroid. It is also a C-type in the MOVIS catalog of the VISTA Hemisphere Survey conducted with the VISTA telescope at Paranal Observatory in Chile. Rotation period and poles In February 1984, a rotational lightcurve of Backlunda was obtained from photometric observations by Richard Binzel. Lightcurve analysis gave a rotation period of hours with a brightness variation of magnitude (). In May 2019, an alternative period determination of hours with an amplitude of magnitude was made by Tom Polakis at the Command Module Observatory in Arizona (). Additional, tentative lightcurves gave a period of () by French amateur astronomer Laurent Bernasconi in July 2004, () by Jean-Gabriel Bosch and Axel Martin in March 2007, and () by Bruno Christmann, David Augustin and Raoul Behrend in July 2019 (). In 2016, a modeled lightcurve gave a concurring sidereal period of hours using data from a large collaboration of individual observers (such as above). The study also determined two spin axes of (42.0°, 44.0°) and (226.0°, 73.0°) in ecliptic coordinates (λ,β). Diameter and albedo According to the surveys carried out by the Japanese Akari satellite and the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer, Backlunda measures () and () kilometers in diameter and its surface has an albedo of () and (), respectively. The Collaborative Asteroid Lightcurve Link assumes a standard albedo for carbonaceous asteroids of 0.057 and derives a diameter of 40.51 kilometers based on an absolute magnitude of 10.69. Alternative mean-diameter measurements published by the WISE team include (), (), (), () and () with corresponding albedos of (), (), (), () and (). Between 2003 and 2009, several asteroid occultations of Backlunda were observed. The best-rated observations from March 2003, October 2005 and August 2008, gave a best-fit ellipse dimension of (), () and (), respectively. These timed observations are taken when the asteroid passes in front of a distant star. References External links Lightcurve Database Query (LCDB), at www.minorplanet.info Dictionary of Minor Planet Names, Google books Asteroids and comets rotation curves, CdR – Geneva Observatory, Raoul Behrend Discovery Circumstances: Numbered Minor Planets (1)-(5000) – Minor Planet Center 000856 Discoveries by Sergei Belyavsky Named minor planets 000856 19160403

3036695

https://en.wikipedia.org/wiki/857%20Glasenappia

857 Glasenappia

857 Glasenappia is a minor planet orbiting the Sun. It was named after Russian astronomer Sergey Glazenap, who was often referred to as "S. de Glasenapp" in pre-Revolution publications. References External links 000857 Discoveries by Sergei Belyavsky Named minor planets 000857 19160406

3036696

https://en.wikipedia.org/wiki/858%20El%20Djeza%C3%AFr

858 El Djezaïr

858 El Djezaïr is a stony asteroid from the asteroid belt, about 24 kilometers in diameter. It was discovered on May 26, 1916, by French astronomer Frédéric Sy at the Algiers Observatory in Algeria, North Africa, and given the provisional designation 1916 a. The asteroid orbits the Sun at a distance of 2.5–3.1 AU once every 4.71 years (1,722 days). The bright S-type asteroid has a very high geometric albedo of 0.32. Its rotation period has been measured to take 22 hours and 20 minutes. Along with the asteroids 68 Leto and 236 Honoria, it is a member of the Leto family, a small, well-defined group of asteroids, all with a semi-major axis of close to 2.8 AU. El Djezaïr is the French spelling of the Arabic name for Algiers, the capital of Algeria. It means "the islands". The asteroid was the first minor planet to receive a name that consists of more than one word. Its designation, 1916 a, is a superseded version of the modern two-letter code system of provisional designation, implemented just a few years later in 1925. References External links Lightcurve plot of 858 El Djezair, Palmer Divide Observatory, B. D. Warner (2005) Asteroid Lightcurve Database (LCDB), query form (info ) Dictionary of Minor Planet Names, Google books Asteroids and comets rotation curves, CdR – Observatoire de Genève, Raoul Behrend Discovery Circumstances: Numbered Minor Planets (1)-(5000) – Minor Planet Center 000858 Discoveries by Frédéric Sy Named minor planets 000858 19160526

3036697

https://en.wikipedia.org/wiki/859%20Bouzar%C3%A9ah

859 Bouzaréah

859 Bouzaréah, provisional designation 1916 c, is a dark asteroid from the asteroid belt about 74 kilometers in diameter. It was discovered by French astronomer Frédéric Sy at the Algiers Observatory in Algeria, North Africa, on 2 October 1916. The asteroid orbits the Sun at a distance of 2.9–3.6 AU about once every 6 years (2,117 days) and rotates around its axis in 23 hours. Its low geometric albedo of 0.047 has been measured by the Infrared Astronomical Satellite, IRAS. The asteroid was named after Bouzaréah, location of the discovering observatory and suburb of the Algerian capital, Algiers. Its designation, 1916 c, is a superseded version of the modern two-letter code system of provisional designation, implemented just a few years later in 1925. References External links Dictionary of Minor Planet Names, Google books 000859 Discoveries by Frédéric Sy Named minor planets 19161002

3036699

https://en.wikipedia.org/wiki/860%20Ursina

860 Ursina

860 Ursina is a minor planet orbiting the Sun that was discovered in 1917 by German astronomer Max Wolf. The origin of the name is unknown. Photometric observations of this asteroid collected during 1999 show a rotation period of 9.386 ± 0.002 hours with a brightness variation of 0.22 magnitude. References External links Lightcurve plot of 860 Ursina, Palmer Divide Observatory, B. D. Warner (1999) Asteroid Lightcurve Database (LCDB), query form (info ) Dictionary of Minor Planet Names, Google books Asteroids and comets rotation curves, CdR – Observatoire de Genève, Raoul Behrend Discovery Circumstances: Numbered Minor Planets (1)-(5000) – Minor Planet Center 000860 Discoveries by Max Wolf Named minor planets 000860 000860 19170122

3036700

https://en.wikipedia.org/wiki/862%20Franzia

862 Franzia

862 Franzia (prov. designation: or ) is a stony background asteroid from the central regions of the asteroid belt. It was discovered by German astronomer Max Wolf at the Heidelberg-Königstuhl State Observatory on 28 January 1917. The common S-type asteroid has a rotation period of 7.5 hours and measures approximately in diameter. It was named after the discoverer's son, Franz Wolf. Orbit and classification Franzia is a non-family asteroid of the main belt's background population when applying the hierarchical clustering method to its proper orbital elements. It orbits the Sun in the central asteroid belt at a distance of 2.6–3.0 AU once every 4 years and 8 months (1,715 days; semi-major axis of 2.8 AU). Its orbit has an eccentricity of 0.08 and an inclination of 14° with respect to the ecliptic. The body's observation arc begins with one of its first observations as at Heidelberg Observatory on 22 January 1903, or 14 years prior to its official discovery observation. Naming This minor planet was named in honor of Franz Wolf, son of the discoverer Max Wolf. The was also mentioned in The Names of the Minor Planets by Paul Herget in 1955 (). It also honors the discoverer's father, Franz Wolf, a physician and amateur astronomer who fostered his son's interest in astronomy by setting up a small observatory in the backyard when Max was sixteen. Physical characteristics In the Bus–Binzel SMASS classification, Franzia is a common, stony S-type asteroid. Rotation period Over the last two decades, numerous photometric observations of Franzia have been proven challenging to determine a well defined rotation period. In August 2018, a rotational lightcurve was obtained from observations by Christophe Demeautis and Raoul Behrend. Lightcurve analysis gave a period of hours with a brightness variation of magnitude (). This result supersedes previous observations. Based on observations taken in September 2004, Brian Warner at his Palmer Divide Observatory , Colorado, published an ambiguous period of and hours with an amplitude of and magnitude, respectively, depending on whether the period solution is derived from a monomodal or from a bimodal lightcurve (). Alternatively, Warner also gave a revised period of hours and an amplitude of magnitude for his other observation taken in December 2000. In February 2011, James W. Brinsfield at the Via Capote Observatory in California measured a period of hours with an amplitude of magnitude (). Observations by Nicolas Esseiva and Raoul Behrend in December 2014 gave a tentative period of hours and a weak amplitude of magnitude (). A basically identical period of hours with a brightness variation of magnitude was determined by French amateur astronomer René Roy in February 2011 (). In March 2016, the Spanish group of asteroid observers, OBAS, measures a period of hours with an amplitude of magnitude (). Diameter and albedo According to the surveys carried out by the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer, the Infrared Astronomical Satellite IRAS, and the Japanese Akari satellite, Franzia measures (), () and () kilometers in diameter and its surface has an albedo of (), () and (), respectively. The Collaborative Asteroid Lightcurve Link derives an albedo of 0.2700 and a diameter of 28.05 kilometers based on an absolute magnitude of 9.8. Notes References External links Lightcurve Database Query (LCDB), at www.minorplanet.info Dictionary of Minor Planet Names, Google books Asteroids and comets rotation curves, CdR – Geneva Observatory, Raoul Behrend Discovery Circumstances: Numbered Minor Planets (1)-(5000) – Minor Planet Center 000862 Discoveries by Max Wolf Named minor planets 000862 19170128

3036704

https://en.wikipedia.org/wiki/863%20Benkoela

863 Benkoela

863 Benkoela is an A-type asteroid orbiting the Sun that was discovered by German astronomer Max Wolf on 9 February 1917 from Heidelberg. 10μ radiometric data collected from Kitt Peak in 1975 gave a diameter estimate of 34 km. References External links Lightcurve plot of 863 Benkoela, Palmer Divide Observatory, B. D. Warner (2004) Asteroid Lightcurve Database (LCDB), query form (info ) Dictionary of Minor Planet Names, Google books Asteroids and comets rotation curves, CdR – Observatoire de Genève, Raoul Behrend Discovery Circumstances: Numbered Minor Planets (1)-(5000) – Minor Planet Center 000863 Discoveries by Max Wolf Named minor planets 000863 000863 19170209

3036707

https://en.wikipedia.org/wiki/864%20Aase

864 Aase

864 Aase is an S-type asteroid belonging to the Flora family in the Main Belt. The object A917 CB discovered 13 February 1917, by Max Wolf was named 864 Aase, and the object 1926 XB discovered 7 December 1926, by Karl Reinmuth was named 1078 Mentha. In 1958 it was discovered that these were one and the same object. In 1974, this was resolved by keeping the name 1078 Mentha and reusing the name and number 864 Aase for the object 1921 KE, discovered 30 September 1921, by Karl Reinmuth. Aase refers to the character from Henrik Ibsen's play Peer Gynt. References External links 000864 Discoveries by Karl Wilhelm Reinmuth Named minor planets 864 Aase 000864 19210930

3036709

https://en.wikipedia.org/wiki/865%20Zubaida

865 Zubaida

865 Zubaida is an elongated, stony background asteroid from the inner regions of the asteroid belt. It was discovered on 15 February 1917, by astronomer Max Wolf at the Heidelberg Observatory in southwest Germany, and given the provisional designations and . The uncommon L-type asteroid has a rotation period of 11.4 hours and measures approximately in diameter. It was named after Zobeide, a character in the opera Abu Hassan by Carl Maria von Weber (1786–1826). Orbit and classification Zubaida is a non-family asteroid of the main belt's background population when applying the hierarchical clustering method to its proper orbital elements. It orbits the Sun in the inner asteroid belt at a distance of 1.9–2.9 AU once every 3 years and 9 months (1,373 days; semi-major axis of 2.42 AU). Its orbit has an eccentricity of 0.19 and an inclination of 13° with respect to the ecliptic. The body's observation arc begins with its first observation as at Heidelberg Observatory on 29 November 1908, more than 8 years prior to its official discovery observation. Naming This minor planet was named after the character Zobeide, the Caliph's wife in the opera Abu Hassan by German composer Carl Maria von Weber (1786–1826). The official was also mentioned in The Names of the Minor Planets by Paul Herget in 1955 (). Another asteroid, 866 Fatme, was also named after one of the characters of this opera. The composer himself was honored with the naming of 4152 Weber. Physical characteristics In the SDSS-based taxonomy (MOC), Zubaida is an uncommon L-type asteroid, while in the Masi Foglia Binzel (MFB) taxonomic variant, it is a common, stony S-type asteroid. Rotation period In January 2007, a rotational lightcurve of Zubaida was obtained from photometric observations by Colin Bembrick at the Mount Tarana Observatory and Greg Crawford at Bagnall Beach Observatory in collaboration with two other Australian observers. Lightcurve analysis gave a well-defined rotation period of hours with a brightness variation of magnitude (). The observers also estimate an axial ratio (a/b) of 1.42 for the asteroid. An alternative observation during January 2007, by David Higgins and Julian Oey at Hunters Hill and Leura observatories, respectively, gave a concurring period hours with an amplitude of magnitude (). Diameter and albedo According to the surveys carried out by the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer (WISE), the Japanese Akari satellite, and the Infrared Astronomical Satellite IRAS, Zubaida measures (), () and () kilometers in diameter and its surface has an albedo of (), () and (), respectively. The WISE team also published an alternative mean-diameter of () with a corresponding albedo of (). The Collaborative Asteroid Lightcurve Link assumes a standard albedo for a stony asteroid of 0.20 and calculates a diameter of 13.58 kilometers based on an absolute magnitude of 11.7. Notes References External links Lightcurve Database Query (LCDB), at www.minorplanet.info Dictionary of Minor Planet Names, Google books Asteroids and comets rotation curves, CdR – Geneva Observatory, Raoul Behrend Discovery Circumstances: Numbered Minor Planets (1)-(5000) – Minor Planet Center 000865 Discoveries by Max Wolf Named minor planets 19170215

3036711

https://en.wikipedia.org/wiki/866%20Fatme

866 Fatme

866 Fatme (prov. designation: or ) is a large background asteroid, approximately in diameter, located in the outer region of the asteroid belt. It was discovered by German astronomer Max Wolf at the Heidelberg-Königstuhl State Observatory on 25 February 1917. The X-type asteroid has a short rotation period of 5.8 hours. It was named after "Fatme", a character in the opera Abu Hassan by Carl Maria von Weber (1786–1826). Orbit and classification Fatme is a non-family asteroid of the main belt's background population when applying the hierarchical clustering method to its proper orbital elements. It orbits the Sun in the outer asteroid belt at a distance of 3.0–3.3 AU once every 5 years and 6 months (2,017 days; semi-major axis of 3.12 AU). Its orbit has an eccentricity of 0.05 and an inclination of 9° with respect to the ecliptic. The body's observation arc begins at Heidelberg Observatory on 16 March 1917, or three weeks after its official discovery observation. Naming This minor planet was named after Fatme, a character in the opera Abu Hassan by German composer Carl Maria von Weber (1786–1826). The official was also mentioned in The Names of the Minor Planets by Paul Herget in 1955 (). Another asteroid 865 Zubaida, was also named after a character of this opera. The composer himself was honored with the naming of 4152 Weber. Physical characteristics In the Bus–Binzel SMASS classification, Fatme is an X-type asteroid. Rotation period In June 2018, a rotational lightcurve of Fatme was obtained from 5 nights of photometric observations by Tom Polakis at the Command Module Observatory in Arizona. Lightcurve analysis gave a rotation period of hours with a brightness variation of magnitude (). The result supersedes previously reported period determinations of hours with an amplitude of magnitude by Robert Stephens at the Santana Observatory , California, in May 2001 (), hours with an amplitude of magnitude (tentative) by French amateur astronomer Laurent Bernasconi in December 2004 (), hours with an amplitude of magnitude (tentative) by French amateur astronomer René Roy in May 2012 (), and hours with an amplitude of magnitude by the Spanish group of asteroid observers, OBAS, in January 2016 (). Diameter and albedo According to the surveys carried out by the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer (WISE), the Japanese Akari satellite, and the Infrared Astronomical Satellite IRAS, Fatme measures (), () and () kilometers in diameter and its surface has an albedo of (), () and (), respectively. The Collaborative Asteroid Lightcurve Link derives an albedo of 0.0361 and a diameter of 88.11 kilometers based on an absolute magnitude of 9.5. Alternative mean-diameter measurements published by the WISE team include (), () and () with corresponding albedos of (), () and (). References External links Lightcurve Database Query (LCDB), at www.minorplanet.info Dictionary of Minor Planet Names, Google books Asteroids and comets rotation curves, CdR – Geneva Observatory, Raoul Behrend Discovery Circumstances: Numbered Minor Planets (1)-(5000) – Minor Planet Center 000866 Discoveries by Max Wolf Named minor planets 000866 19170225

3036715

https://en.wikipedia.org/wiki/867%20Kovacia

867 Kovacia

867 Kovacia (prov. designation: or ) is an elongated, dark asteroid and member of the Hygiea family from the outer regions of the asteroid belt. It was discovered on 25 February 1917, by astronomer Johann Palisa at the Vienna Observatory in Austria. The carbonaceous C/B-type asteroid has a rotation period of 8.7 hours and measures approximately in diameter. It was named after Austrian physician Friedrich Kovacs (1861–1931). Orbit and classification According to Zappalà's classification of dynamical families, and when applying the synthetic hierarchical clustering method (HCM) by Nesvorný, Kovacia is a member of the Hygiea family (), a very large family of carbonaceous outer-belt asteroids, named after 10 Hygiea, which is the main belt's fourth-largest asteroid. However, it is a non-family background asteroid according to another HCM-analysis by Milani and Knežević (AstDys). It orbits the Sun in the outer asteroid belt at a distance of 2.7–3.5 AU once every 5 years and 4 months (1,961 days; semi-major axis of 3.07 AU). Its orbit has an eccentricity of 0.13 and an inclination of 6° with respect to the ecliptic. The body's observation arc begins at Vienna Observatory on 1 March 1917, or four nights after its official discovery observation. Naming This minor planet was named by Palisa after Friedrich Kovacs (1861–1931), a Vienna physician and internists, who successfully treated and restored the health of the discoverer's wife. The famed Viennese cardiologist also treated Gustav Mahler, who had a defective heart. Kovacs imposed a curtailment of all forms of vigorous exercise, a strict regimen of rest and even the usage of a pedometer to measure the composer's physical effort. These restrictions depressed Mahler and ultimately lead to the Symphony No. 9, his last completed work. The was also mentioned in The Names of the Minor Planets by Paul Herget in 1955 (). Physical characteristics In the SDSS-based taxonomy, Kovacia is a dark and common carbonaceous C-type asteroid, while in a spectroscopic study of the Hygiea family from 2001, this asteroid has been classified as a somewhat brighter B-type asteroid. The study finds a significant number of objects of this family to belong to this spectral type. Both C/B-types agree with the overall spectral type for the Hygiea family listed by Nesvorný (). Rotation period and poles In February 2008, a rotational lightcurve of Kovacia was obtained from photometric observations by a collaboration of French and Italian amateur astronomers including René Roy, Silvano Casulli, François Colas, Arnaud Leroy, Federico Manzini, Christophe Demeautis and Jean-François Coliac. Lightcurve analysis gave a well-defined rotation period of hours with a high brightness variation of magnitude, indicative of a non-spherical, elongated shape (). The result supersedes a previous observation by Roberto Crippa and Federico Manzini at the Sozzago Astronomical Station from November 2006, that determined a lower limit of 6 hours (). Due to observed mutual occultation and eclipsing events, the collaboration of astronomers strongly suspect Kovacia to be a binary asteroid with a satellite orbiting it every days. However, no follow-up observations have been published. , this asteroid is neither listed at Johnstons Archive nor has it any kind of binary status in the Lightcurve Data Base. In 2016, a modeled lightcurve gave a concurring sidereal period of hours using data from the Uppsala Asteroid Photometric Catalogue, the Palomar Transient Factory survey, and individual observers (such as above), as well as sparse-in-time photometry from the NOFS, the Catalina Sky Survey, and the La Palma surveys . The study also determined two spin axes of (200.0°, −44.0°) and (38.0°, −50.0°) in ecliptic coordinates (λ, β). Diameter and albedo According to the surveys carried out by the Infrared Astronomical Satellite IRAS, the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer (WISE), and the Japanese Akari satellite, Kovacia measures (), () and () kilometers in diameter and its surface has an albedo of (), () and (), respectively. The Collaborative Asteroid Lightcurve Link derives an albedo of 0.0772 and a diameter of 23.96 kilometers based on an absolute magnitude of 11.5. Alternative mean-diameter measurements published by the WISE team include () and () with corresponding albedos of () and (). References External links Kovacs, Friedrich (1861–1931), Internist, Institut für Neuzeit- und Zeitgeschichtsforschung Lightcurve Database Query (LCDB), at www.minorplanet.info Dictionary of Minor Planet Names, Google books Asteroids and comets rotation curves, CdR – Geneva Observatory, Raoul Behrend Discovery Circumstances: Numbered Minor Planets (1)-(5000) – Minor Planet Center 000867 Discoveries by Johann Palisa Named minor planets 19170225

3036717

https://en.wikipedia.org/wiki/868%20Lova

868 Lova

868 Lova (prov. designation: or ) is a large and dark background asteroid, approximately in diameter, from the central regions of the asteroid belt. It was discovered by German astronomer Max Wolf at the Heidelberg-Königstuhl State Observatory on 26 April 1917. The carbonaceous C-type asteroid (Ch) and has a long rotation period of 41.1 hours and is likely elongated in shape. The origin of the asteroid's name remains unknown. Orbit and classification Lova is a non-family asteroid of the main belt's background population when applying the hierarchical clustering method to its proper orbital elements. It orbits the Sun in the central asteroid belt at a distance of 2.3–3.1 AU once every 4 years and 5 months (1,624 days; semi-major axis of 2.7 AU). Its orbit has an eccentricity of 0.15 and an inclination of 6° with respect to the ecliptic. The body's observation arc begins at Heidelberg Observatory on 3 March 1930, almost 13 years after its official discovery observation. Naming This minor planet was named by the discoverer. Any reference of this name to a person or occurrence is unknown. Unknown meaning Among the many thousands of named minor planets, Lova is one of 120 asteroids, for which no official naming citation has been published. All of these low-numbered asteroids have numbers between and and were discovered between 1876 and the 1930s, predominantly by astronomers Auguste Charlois, Johann Palisa, Max Wolf and Karl Reinmuth. Physical characteristics In the Tholen classification, Lova is a common, dark C-type asteroid with a noisy spectrum (:), while in the Bus–Binzel SMASS classification, it is a hydrated, carbonaceous subtype (Ch). Rotation period In November 2017, a rotational lightcurve of Lova was obtained from photometric observations by Tom Polakis at the Command Module Observatory in Arizona. Lightcurve analysis gave a well-defined rotation period of hours with a brightness variation of magnitude (). While not being a slow rotator, which have periods of 100 or more hours, Lovas period is significantly longer than the vast majority of asteroids, which rotate within 2.2 to 20 hours once around their axis. A lower-rated lightcurve by French amateur astronomer Laurent Bernasconi gave a similar period of hours with a higher amplitude of magnitude, indicative of an elongated shape (). The results supersede a period determination with a lower limit of hours and amplitude of at least magnitude by Brian Warner at his Palmer Divide Observatory in Colorado from November 1999 (). In 2006, Warner revised his photometric data, though with no notable improvement or change for this asteroid. Diameter and albedo According to the surveys carried out by the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer (WISE), the Infrared Astronomical Satellite IRAS, and the Japanese Akari satellite, Lova measures (), () and () kilometers in diameter and its surface has an albedo of (), () and (), respectively. The Collaborative Asteroid Lightcurve Link adopts the results from IRAS, that is, a low albedo of 0.0524 and a diameter of 52.47 kilometers based on an absolute magnitude of 10.22. Alternative mean-diameter measurements published by the WISE team include (), (), () and () with corresponding albedos of (), (), () and (). Two asteroid occultations, observed on 5 April 2006 and 12 July 2007, gave a best-fit ellipse dimension of (52.0 × 52.0) and (43.3 × 64.3) kilometers, respectively, with the latter being the better rated one. These timed observations are taken when the asteroid passes in front of a distant star. Notes References External links Lightcurve Database Query (LCDB), at www.minorplanet.info Dictionary of Minor Planet Names, Google books Asteroids and comets rotation curves, CdR – Geneva Observatory, Raoul Behrend Discovery Circumstances: Numbered Minor Planets (1)-(5000) – Minor Planet Center 000868 Discoveries by Max Wolf Named minor planets 000868 000868 19170426

3036719

https://en.wikipedia.org/wiki/869%20Mellena

869 Mellena

869 Mellena (prov. designation: or ) is a dark background asteroid from the central region of the asteroid belt. It was discovered on 9 May 1917, by astronomer Richard Schorr at the Bergedorf Observatory in Hamburg. The carbonaceous C-type asteroid has a shorter than average rotation period of 6.5 hours and measures approximately in diameter. It was named after Werner von Melle (1853–1937), mayor of Hamburg, who founded the discovering observatory. Orbit and classification Mellena is a non-family asteroid of the main belt's background population when applying the hierarchical clustering method to its proper orbital elements. It orbits the Sun in the central asteroid belt at a distance of 2.1–3.3 AU once every 4 years and 5 months (1,610 days; semi-major axis of 2.69 AU). Its orbit has an eccentricity of 0.22 and an inclination of 8° with respect to the ecliptic. Discovery Mellena was discovered by German astronomer Richard Schorr at the Bergedorf Observatory in Hamburg on 9 May 1917. On the following night, it was independently discovered by Max Wolf at Heidelberg Observatory on 10 May 1917. The Minor Planet Center, however, only credits the first discoverer. Schorr only discovered one more asteroid, 1240 Centenaria, and was honored with the naming of Mars-crosser 1235 Schorria, discovered by Wolf. Mellenas observation arc begins at Algiers Observatory in Northern Africa on 26 March 1930, almost 13 years after its official discovery observation at Bergedorf. Naming This minor planet was named after Werner von Melle (1853–1937), who was the mayor of Hamburg, Germany, in 1915 and during 1918–1919. He promoted the establishment of the University of Hamburg and founded the Bergedorf–Hamburg Observatory where this minor planet was discovered. The was also mentioned in The Names of the Minor Planets by Paul Herget in 1955 (). Physical characteristics In both the Tholen- and SMASS-like taxonomy of the Small Solar System Objects Spectroscopic Survey (S3OS2) as well as in the SDSS-based taxonomy, Mellena is a common, carbonaceous C-type asteroid. Rotation period In May 2010, a rotational lightcurve of Mellena was obtained from photometric observations by Robert Stephens at the Santana and GMARS observatories in California. Lightcurve analysis gave a well-defined rotation period of hours with a brightness variation of magnitude (). Subsequent observations were taken by Andrea Ferrero at the Bigmuskie Observatory in Mombercelli, Italy (), and Larry Owings at the Barnes Ridge Observatory in California in June 2010 (), as well as by Albino Carbognani Astronomical at the OAVdA Observatory in July 2010 (). These observations gave a concurring period of (), () and () hours with an amplitude of (), () and () magnitude, respectively. Diameter and albedo According to the surveys carried out by the Japanese Akari satellite, the Infrared Astronomical Satellite IRAS, and the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer (WISE), Mellena measures (), () and () kilometers in diameter and its surface has an albedo of (), () and (), respectively. The Collaborative Asteroid Lightcurve Link derives an albedo of 0.0884 and a diameter of 18.64 kilometers based on an absolute magnitude of 11.9. Alternative mean-diameter measurements published by the WISE team include (), (), () and () with corresponding albedos of (), (), () and (). References External links Lightcurve Database Query (LCDB), at www.minorplanet.info Dictionary of Minor Planet Names, Google books Discovery Circumstances: Numbered Minor Planets (1)-(5000) – Minor Planet Center 000869 Discoveries by Richard Schorr Named minor planets 19170509

3036726

https://en.wikipedia.org/wiki/871%20Amneris

871 Amneris

871 Amneris is a minor planet orbiting the Sun. It is the namesake of the Amneris family, a subgroup of the Flora family of Main Belt asteroids. This asteroid was named after Amneris, a character in Giuseppe Verdi's Aida. References External links Asteroid 871 Amneris, Small Bodies Data Ferret 000871 000871 Discoveries by Max Wolf Named minor planets Giuseppe Verdi 19170514

3036729

https://en.wikipedia.org/wiki/872%20Holda

872 Holda

872 Holda is a minor planet orbiting the Sun. The asteroid is named after Edward Singleton Holden, an American astronomer. References External links 000872 Discoveries by Max Wolf Named minor planets 000872 000872 19170521

3036730

https://en.wikipedia.org/wiki/870%20Manto

870 Manto

870 Manto (prov. designation: or ) is a stony background asteroid and slow rotator from the inner region of the asteroid belt. It was discovered on 12 May 1917, by astronomer Max Wolf at the Heidelberg Observatory in southwest Germany. The likely heavily elongated S-type asteroid has a long rotation period of 122.3 hours and measures approximately in diameter. It was named after Manto, a prophetess in Greek mythology. Orbit and classification Manto is a non-family asteroid of the main belt's background population when applying the hierarchical clustering method to its proper orbital elements. It orbits the Sun in the inner asteroid belt at a distance of 1.7–2.9 AU once every 3 years and 6 months (1,293 days; semi-major axis of 2.32 AU). Its orbit has an eccentricity of 0.27 and an inclination of 6° with respect to the ecliptic. The asteroid was first observed as () at Taunton Observatory on 11 October 1907, and again as () at the Simeiz Observatory on 16 October 1914. The body's observation arc begins with its official discovery observation at Heidelberg Observatory on 12 May 1917. Naming This minor planet was named after Manto from Greek mythology. She was the daughter of Teresias Thebanus and a famous soothsayer, who erected of a temple of Apollo (Apollo Clarius) in Claros. The was also mentioned in The Names of the Minor Planets by Paul Herget in 1955 (). Physical characteristics Manto is a common stony S-type asteroid in the Bus–Binzel SMASS classification, and in both the Tholen- and SMASS-like taxonomy of the Small Solar System Objects Spectroscopic Survey (S3OS2). Rotation period In September 2013, a rotational lightcurve of Manto was obtained from photometric observations by Frederick Pilcher at the Organ Mesa Observatory , New Mexico, in collaboration with Eduardo Manuel Alvarez, Andrea Ferrero, Daniel Klinglesmith and Julian Oey Lightcurve analysis gave an exceptionally long rotation period of hours with a notably high brightness amplitude of magnitude, indicative of an elongated shape (). With a period above 100 hours, the asteroid is a slow rotator. The result supersedes observations by Alain W. Harris from July 1981, and by astronomers at the Intermediate Palomar Transient Factory in California (). In 2016, a modeled lightcurve gave a concurring sidereal period of hours using data from a large collaboration of individual observers (such as above). The study also determined two spin axes of (96.0°, 30.0°) and (283.0°, 35.0°) in ecliptic coordinates (λ, β). Diameter and albedo According to the surveys carried out by the Japanese Akari satellite and the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer (WISE), Manto measures () and () kilometers in diameter and its surface has an albedo of () and (), respectively. The Collaborative Asteroid Lightcurve Link assumes a standard albedo for a stony asteroid of 0.20 and calculates a diameter of 13.71 kilometers based on an absolute magnitude of 11.68. The WISE team also published an alternative mean-diameter measurement of () with a corresponding albedo of (). References External links Lightcurve Database Query (LCDB), at www.minorplanet.info Dictionary of Minor Planet Names, Google books Discovery Circumstances: Numbered Minor Planets (1)-(5000) – Minor Planet Center 000870 Discoveries by Max Wolf Named minor planets 000870 000870 19170512

3036735

https://en.wikipedia.org/wiki/874%20Rotraut

874 Rotraut

874 Rotraut (prov. designation: or ) is a dark and elongated background asteroid, approximately in diameter, located in the outer region of the asteroid belt. It was discovered on 25 May 1917, by astronomer Max Wolf at the Heidelberg-Königstuhl State Observatory is southwest Germany. The hydrated carbonaceous C-type asteroid (Ch) has a rotation period of 14.3 hours. It was likely named after the ballad Schön Rotraut by German lyric poet Eduard Mörike (1804–1875). Orbit and classification Rotraut is a non-family asteroid of the main belt's background population when applying the hierarchical clustering method to its proper orbital elements. It orbits the Sun in the outer asteroid belt at a distance of 2.9–3.4 AU once every 5 years and 7 months (2,044 days; semi-major axis of 3.15 AU). Its orbit has an eccentricity of 0.08 and an inclination of 11° with respect to the ecliptic. The body's observation arc begins at Heidelberg Observatory with its official discovery observation on 25 May 1917. Naming "Rotraut" is a feminine German first name. This minor planet was likely named after the ballad Schön Rotraut (Pretty Rohtraut) by the German lyric poet Eduard Mörike (1804–1875). Lutz Schmadel, the author of the Dictionary of Minor Planet Names learned about Wolf's source of inspiration from private communications with Dutch astronomer Ingrid van Houten-Groeneveld, who worked as a young astronomer at Heidelberg. Physical characteristics In the Tholen-like taxonomy of the Small Solar System Objects Spectroscopic Survey (S3OS2), Rotraut is a carbonaceous C-type asteroid (Caa), while in the survey's SMASS-like taxonomic variation it is a hydrated C-type (Ch). Rotation period Two rotational lightcurves of Rotraut were obtained from photometric observations by Richard Ditteon at Oakley Southern Sky Observatory , Australia, in February 2017, and by Tom Polakis at the Command Module Observatory in Arizona in May 2018. Lightcurve analysis gave an identical rotation period of hours with a brightness variation of and magnitude, respectively (). The result supersedes a tentative period determination of hours and an amplitude of magnitude by French amateur astronomers Stéphane Charbonnel and Claudine Rinner from July 2002 (). In 2016, a modeled lightcurve gave a sidereal period of hours using data from the Uppsala Asteroid Photometric Catalogue, the Palomar Transient Factory survey, and individual observers (such as above), as well as sparse-in-time photometry from the NOFS, the Catalina Sky Survey, and the La Palma surveys . The study also determined two spin axes of (201.0°, −41.0°) and (2.0°, −36.0°) in ecliptic coordinates (λ, β). Diameter and albedo According to the surveys carried out by the Infrared Astronomical Satellite IRAS, the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer (WISE), and the Japanese Akari satellite, Rotraut measures (), () and () kilometers in diameter and its surface has an albedo of (), () and (), respectively. The Collaborative Asteroid Lightcurve Link derives an albedo of 0.0506 and a diameter of 56.42 kilometers based on an absolute magnitude of 10.1. Alternative mean-diameter measurements published by the WISE team include (), (), () and () with corresponding albedos of (), (), () and (). Three asteroid occultations, observed on 30 November 2009, 22 September 2013 and 21 November 2015, gave a best-fit ellipse dimension of (), () (best), and (), respectively. These timed observations are taken when the asteroid passes in front of a distant star. However the quality of the measurement is rated poorly. References External links Pretty Rohtraut, The LiederNet Archive Lightcurve Database Query (LCDB), at www.minorplanet.info Dictionary of Minor Planet Names, Google books Asteroids and comets rotation curves, CdR – Geneva Observatory, Raoul Behrend Discovery Circumstances: Numbered Minor Planets (1)-(5000) – Minor Planet Center 000874 Discoveries by Max Wolf Named minor planets 19170525

3036736

https://en.wikipedia.org/wiki/873%20Mechthild

873 Mechthild

873 Mechthild (prov. designation: or ) is a dark background asteroid from the central regions of the asteroid belt. It was discovered by German astronomer Max Wolf at the Heidelberg Observatory on 21 May 1917. The primitive P-type asteroid has a rotation period of 11.0 hours and measures approximately in diameter. The origin of the asteroid's name remains unknown. Orbit and classification Mechthild is a non-family asteroid of the main belt's background population when applying the hierarchical clustering method to its proper orbital elements. It orbits the Sun in the central asteroid belt at a distance of 2.2–3.0 AU once every 4 years and 3 months (1,555 days; semi-major axis of 2.63 AU). Its orbit has an eccentricity of 0.15 and an inclination of 5° with respect to the ecliptic. The body's observation arc begins with its first and official discovery observation at Heidelberg Observatory on 21 May 1917. Naming This minor planet is named "Mechthild", a German feminine given name. Any reference of this name to a specific person or occurrence is unknown. Unknown meaning Among the many thousands of named minor planets, Mechthild is one of 120 asteroids, for which no official naming citation has been published. All of these low-numbered asteroids have numbers between and and were discovered between 1876 and the 1930s, predominantly by astronomers Auguste Charlois, Johann Palisa, Max Wolf and Karl Reinmuth. Physical characteristics In the Tholen classification, Mechthild is closest to a very dark, primitive P-type, and somewhat similar to a common C-type asteroid. In the taxonomy by Barucci, it is a C0-type. P-type asteroids are more common in the outer asteroid belt and among the Jupiter trojan population. Rotation period In May 2015, a rotational lightcurve of Mechthild was obtained from photometric observations by Brian Warner at his Palmer Divide Observatory in Colorado. Lightcurve analysis gave a rotation period of hours with a brightness amplitude of magnitude (). Alternative period determinations were made by Claes-Ingvar Lagerkvist () in March 1976, by astronomers at the Palomar Transient Factory () in January 2014, and by the Spanish group of asteroid observers, OBAS () in May 2015 (). In 2016, a modeled lightcurve gave a concurring sidereal period of hours using data from a large collaboration of individual observers (such as above). The study also determined two spin axes of (249.0°, −52.0°) and (51.0°, −61.0°) in ecliptic coordinates (λ, β). Diameter and albedo According to the surveys carried out by the Infrared Astronomical Satellite IRAS, and the Japanese Akari satellite, and the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer (WISE), Mechthild measures (), () and () kilometers in diameter and its surface has an albedo of (), () and (), respectively. The Collaborative Asteroid Lightcurve Link adopts the results from IRAS, that is, an albedo of 0.0531 and a diameter of 29.04 kilometers based on an absolute magnitude of 11.49. Alternative mean-diameter measurements published by the WISE team include () and () with corresponding albedos of () and (). References External links Lightcurve Database Query (LCDB), at www.minorplanet.info Dictionary of Minor Planet Names, Google books Discovery Circumstances: Numbered Minor Planets (1)-(5000) – Minor Planet Center 000873 Discoveries by Max Wolf Named minor planets 000873 19170521

3036738

https://en.wikipedia.org/wiki/875%20Nymphe

875 Nymphe

875 Nymphe is a minor planet orbiting the Sun. It is a member of the Maria family of asteroids. References External links Lightcurve plot of 875 Nymphe, Palmer Divide Observatory, B. D. Warner (2003) Asteroid Lightcurve Database (LCDB), query form (info ) Dictionary of Minor Planet Names, Google books Asteroids and comets rotation curves, CdR – Observatoire de Genève, Raoul Behrend Discovery Circumstances: Numbered Minor Planets (1)-(5000) – Minor Planet Center 000875 Discoveries by Max Wolf Named minor planets 19170519

3036739

https://en.wikipedia.org/wiki/876%20Scott

876 Scott

876 Scott is a minor planet orbiting the Sun. For a long time, its name had been falsely attributed to Robert Falcon Scott. In fact, it was named after discoverer Johann Palisa's financial supporter Miss E. Scott. References External links 000876 Discoveries by Johann Palisa Named minor planets 000876 19170620

3036742

https://en.wikipedia.org/wiki/877%20Walk%C3%BCre

877 Walküre

877 Walküre (prov. designation: or ) is a dark background asteroid from the inner regions of the asteroid belt, approximately in diameter. It was discovered on 13 September 1915, by Russian astronomer Grigory Neujmin at the Simeiz Observatory on the Crimean peninsula. The carbonaceous F/C-type asteroid has a rotation period of 17.4 hours and is likely elongated in shape. It was named after the female spirit Valkyrie from Norse mythology, best known from Wagner's opera Die Walküre. Orbit and classification Located in or near the orbital region of the Nysa family, Walküre is a non-family asteroid of the main belt's background population when applying the hierarchical clustering method to its proper orbital elements. It orbits the Sun in the inner asteroid belt at a distance of 2.1–2.9 AU once every 3 years and 11 months (1,432 days; semi-major axis of 2.49 AU). Its orbit has an eccentricity of 0.16 and an inclination of 4° with respect to the ecliptic. The asteroid was first observed as () at Heidelberg Observatory on 9 April 1909, where the body's observation arc begins on 25 February 1921, more than 5 years after its official discovery observation at Simeiz on 13 September 1915. Naming This minor planet was named after the Valkyrie () a female spirit from Norse mythology. The shield-bearing valkyries decide the fate of warriors in battle, and conduct some of them to Valhalla, the afterlife hall where the fallen heroes are received. Die Walküre (The Valkyrie) is also part of the opera cycle Der Ring des Nibelungen by Richard Wagner (1813–1883), the others being The Rhinegold, Siegfried and the Twilight of the Gods. The asteroid was named by astronomer Sergey Belyavsky and the was published in the journal Astronomische Nachrichten in 1923 (). Asteroids 894 Erda and 890 Waltraut are also named after characters in Wagner's Ring, while 3992 Wagner and 1260 Walhalla are named after the composer and the Walhalla memorial hall of fame, respectively. Physical characteristics In the Tholen classification, Walküre is a dark, carbonaceous F-type asteroid, while in the SDSS-based taxonomy and in the Barucci-taxonomy, it is a common carbonaceous C-type and C0-type asteroid, respectively. Rotation period In February 2011, a rotational lightcurve of Walküre was obtained from photometric observations by astronomer Li Bin at the XuYi Station of the Purple Mountain Observatory in China. Lightcurve analysis gave a rotation period of hours with a brightness variation of magnitude, indicative of an elongated shape (). The result supersedes observations by Richard Binzel (1982) and René Roy (2005), who determined a period of and with an amplitude of and magnitude, respectively (). Poles Two lightcurves, published in 2016, using modeled photometric data from the Lowell Photometric Database (LPD) and other sources, gave a concurring sidereal period of and hours, respectively. Each modeled lightcurve also determined two spin axes of (68.0°, 58.0°) and (253.0°, 61.0°), as well as (262.0°, 71.0°) and (47.0°, 66.0°) in ecliptic coordinates (λ,β). Diameter and albedo According to the surveys carried out by the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer (WISE), the Japanese Akari satellite, and the Infrared Astronomical Satellite IRAS, Walküre measures (), () and () kilometers in diameter and its surface has an albedo of (), () and (), respectively. The Collaborative Asteroid Lightcurve Link derives an albedo of 0.0634 and gives a diameter of 38.41 kilometers (identical to IRAS) based on an absolute magnitude of 10.69. Alternative mean-diameter measurements published by the WISE team include () and () with corresponding albedos of () and (). References External links Lightcurve Database Query (LCDB), at www.minorplanet.info Dictionary of Minor Planet Names, Google books Asteroids and comets rotation curves, CdR – Geneva Observatory, Raoul Behrend Discovery Circumstances: Numbered Minor Planets (1)-(5000) – Minor Planet Center 000877 Discoveries by Grigory Neujmin Named minor planets 000877 19150913

3036745

https://en.wikipedia.org/wiki/878%20Mildred

878 Mildred

878 Mildred is a minor planet in the main belt orbiting the Sun. It is the lowest numbered, and thus the namesake, of the Mildred family of asteroids, a subgroup of the Nysa family. The Mildred subgroup, and by extension 878 Mildred itself, is thought to have been formed by a recent fragmentation event from a larger asteroid. Discovery 878 Mildred was originally discovered in 1916 using the 1.5 m Hale Telescope at the Mount Wilson Observatory, but was subsequently lost until it was again observed on single nights in 1985 and 1991 (a lost asteroid). Initially only two observations of the asteroid were taken on 1916-09-06 which does not allow for an accurate orbital determination, however interest in the object prompted further investigation and more measurements were taken in late September and October. The asteroid was re-discovered in 1991 by Gareth V. Williams. It is named after Mildred Shapley Matthews. Physical properties By comparing the asteroid's perceived brightness and the then computed distance from the Sun they arrived at an absolute visual magnitude of 14.3, which if one assumes Mars-like albedo gives an approximate diameter of 3 to 5 kilometers. References External links Minor Planet Center Database entry on (878) Mildred 000878 Discoveries by Seth Nicholson Discoveries by Harlow Shapley Named minor planets 19160906

3036748

https://en.wikipedia.org/wiki/879%20Ricarda

879 Ricarda

879 Ricarda is a minor planet orbiting the Sun that was discovered by German astronomer Max Wolf on July 22, 1917. This is a member of the dynamic Maria family of asteroids that most likely formed as the result of a collisional breakup of a parent body. It is named after German intellectual Ricarda Huch. Main-belt asteroid 8847 Huch is also named after her. References External links 000879 Discoveries by Max Wolf Named minor planets 19170722

3036750

https://en.wikipedia.org/wiki/880%20Herba

880 Herba

880 Herba is a minor planet orbiting the Sun that was discovered by German astronomer Max Wolf on 22 July 1917 in Heidelberg. Photometric observations of this asteroid at the Organ Mesa Observatory in Las Cruces, New Mexico, in 2011 gave a light curve with a period of 12.266 ± 0.001 hours and a brightness variation of 0.13 ± 0.02 in magnitude. The curve is asymmetrical with one maxima and one minima. 880 Herba is named after Herba, the Greek god of misery and poverty. References External links Lightcurve plot of 880 Herba, Palmer Divide Observatory, B. D. Warner (2006) Asteroid Lightcurve Database (LCDB), query form (info ) Dictionary of Minor Planet Names, Google books Asteroids and comets rotation curves, CdR – Observatoire de Genève, Raoul Behrend Discovery Circumstances: Numbered Minor Planets (1)-(5000) – Minor Planet Center 000880 Discoveries by Max Wolf Named minor planets 000880 19170722

3036756

https://en.wikipedia.org/wiki/882%20Swetlana

882 Swetlana

882 Swetlana (prov. designation: or ) is a dark background asteroid from the outer region of the asteroid belt. It was discovered on 15 August 1917, by Russian astronomer Grigory Neujmin at the Simeiz Observatory on the Crimean peninsula. The X-type asteroid has a longer-than average rotation period of 29.9 hours and measures approximately in diameter. The origin of the asteroid's name remains unknown. Orbit and classification Swetlana is a non-family asteroid of the main belt's background population when applying the hierarchical clustering method to its proper orbital elements. It orbits the Sun in the outer asteroid belt at a distance of 2.3–4.0 AU once every 5 years and 6 months (2,016 days; semi-major axis of 3.12 AU). Its orbit has an eccentricity of 0.27 and an inclination of 6° with respect to the ecliptic. The body's observation arc begins on 18 August 1917, with its independent discovery at Heidelberg Observatory by Max Wolf, just three nights after its official discovery observation by Grigory Neujmin at Simeiz. Naming This minor planet is named after a Feminine Russian first name. Any reference of this name to a person or occurrence is unknown. Unknown meaning Among the many thousands of named minor planets, Swetlana is one of 120 asteroids, for which no official naming citation has been published. All of these low-numbered asteroids have numbers between and and were discovered between 1876 and the 1930s, predominantly by astronomers Auguste Charlois, Johann Palisa, Max Wolf and Karl Reinmuth. Physical characteristics In both the Tholen- and SMASS-like taxonomy of the Small Solar System Objects Spectroscopic Survey (S3OS2), Swetlana is an X-type asteroid. Rotation period In September 2017, a rotational lightcurve of Swetlana was obtained from photometric observations by Thomas A. Polakis at the Command Module Observatory in Arizona. Lightcurve analysis gave a well-defined rotation period of hours with a brightness variation of magnitude (). The result supersedes an observations by Italian amateur astronomers Roberto Crippa and Federico Manzini at the Sozzago Astronomical Station from September 2006, which tentatively determined a period of more than 20 hours and an amplitude of magnitude (). Diameter and albedo According to the surveys carried out by the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer (WISE), the Infrared Astronomical Satellite IRAS, and the Japanese Akari satellite, Swetlana measures (), () and () kilometers in diameter and its surface has an albedo of (), () and (), respectively. The Collaborative Asteroid Lightcurve Link derives an albedo of 0.0491 and a diameter of 43.47 kilometers based on an absolute magnitude of 10.7. Alternative measurements published by the WISE team include mean-diameters of () and () with corresponding albedos of () and (). References External links Lightcurve Database Query (LCDB), at www.minorplanet.info Dictionary of Minor Planet Names, Google books Asteroids and comets rotation curves, CdR – Geneva Observatory, Raoul Behrend Discovery Circumstances: Numbered Minor Planets (1)-(5000) – Minor Planet Center 000882 Discoveries by Grigory Neujmin Named minor planets 19170815

3036757

https://en.wikipedia.org/wiki/881%20Athene

881 Athene

881 Athene (prov. designation: or ) is a stony background asteroid from the central region of the asteroid belt. It was discovered on 22 July 1917, by astronomer Max Wolf at the Heidelberg-Königstuhl State Observatory in southwest Germany. The likely elongated S/L-type asteroid has a rotation period of 13.9 hours and measures approximately in diameter. It was named after Athena, the goddess of wisdom in Greek mythology. Orbit and classification Located in or near the orbital region of the Eunomia family, Athene is a non-family asteroid of the main belt's background population when applying the hierarchical clustering method to its proper orbital elements. It orbits the Sun in the central asteroid belt at a distance of 2.1–3.2 AU once every 4 years and 3 months (1,543 days; semi-major axis of 2.61 AU). Its orbit has an eccentricity of 0.21 and an inclination of 14° with respect to the ecliptic. The body's observation arc begins at Uccle Observatory on 8 August 1934, almost 17 years after its official discovery observation at Heidelberg on 22 July 1917. Naming This minor planet was named after Athena or "Pallas Athene", the goddess of wisdom in Greek mythology, also known as Minerva in Roman mythology. The was mentioned in The Names of the Minor Planets by Paul Herget in 1955 (). Asteroids 93 Minerva and 2 Pallas are both named after the goddess as well. Physical characteristics In the Tholen-like taxonomy of the Small Solar System Objects Spectroscopic Survey (S3OS2), Athene is a common, stony S-type asteroid, while in the SDSS-based taxonomy, it is an L-type asteroid. In the SMASS-like taxonomic variant of the S3OS2, Athene is an Sl-subtype that transitions between the S-and L-type. Rotation period In August 2006, a rotational lightcurve of Athene was obtained from photometric observations by Roberto Crippa and Federico Manzini at the Sozzago Astronomical Station , Italy, and by Jean-Gabriel Bosch at the Collonges Observatory , France. Lightcurve analysis gave a rotation period of hours with a high brightness variation of magnitude, indicative of a non-spherical, elongated shape (). In September 2010, French amateur astronomer René Roy measured a similar period of hours and an amplitude of (). Poles Two lightcurves, published in 2016, using modeled photometric data from the Lowell Photometric Database (LPD) and other sources, gave a concurring sidereal period of and hours, respectively. Each modeled lightcurve also determined two spin axes of (123.0°, −58.0°) and (337.0°, −47.0°), as well as (115.0°, −77.0°) and (338.0°, −43.0°) in ecliptic coordinates (λ, β). Diameter and albedo According to the surveys carried out by the Japanese Akari satellite and the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer (WISE), Athene measures () and () kilometers in diameter and its surface has an albedo of () and (), respectively. The Collaborative Asteroid Lightcurve Link assumes a standard Eunomian albedo of 0.21 and calculates a diameter of 12.66 kilometers based on an absolute magnitude of 11.8. Alternative mean-diameter measurements published by the WISE team include (), () and () with corresponding albedos of (), () and (). References External links Lightcurve Database Query (LCDB), at www.minorplanet.info Dictionary of Minor Planet Names, Google books Asteroids and comets rotation curves, CdR – Geneva Observatory, Raoul Behrend Discovery Circumstances: Numbered Minor Planets (1)-(5000) – Minor Planet Center 000881 Discoveries by Max Wolf Named minor planets 19170722

3036761

https://en.wikipedia.org/wiki/883%20Matterania

883 Matterania

883 Matterania is an S-type asteroid belonging to the Flora family in the Main Belt. Its rotation period is 5.64 hours References External links 000883 000883 Discoveries by Max Wolf Named minor planets 000883 19170914

3036763

https://en.wikipedia.org/wiki/884%20Priamus

884 Priamus

884 Priamus is a large Jupiter trojan from the Trojan camp, approximately in diameter. It was discovered on 22 September 1917, by German astronomer Max Wolf at Heidelberg Observatory in southern Germany. The dark D-type asteroid is one of the 20 largest Jupiter trojans and has a rotation period of 6.9 hours. It was named after the Trojan king Priam from Greek mythology. Orbit and classification Priamus is orbiting in the trailing Trojan camp, at Jupiter's Lagrangian point, 60° behind its orbit in a 1:1 resonance . It is also a non-family asteroid of the Jovian background population. It orbits the Sun at a distance of 4.5–5.8 AU once every 11 years and 10 months (4,308 days; semi-major axis of 5.18 AU). Its orbit has an eccentricity of 0.12 and an inclination of 9° with respect to the ecliptic. The body's observation arc begins at Heidelberg in November 1917, two months after its official discovery observation. Naming This minor planet was named from Greek mythology after Priam (Priamus; Priamos), the king of Troy during the Trojan War. The Jupiter trojans 624 Hektor and 3317 Paris are named after his sons Paris and Hector. The official naming of Ajax was first cited in The Names of the Minor Planets by Paul Herget in 1955 (). Physical characteristics In the Tholen taxonomy, Priamus is a dark D-type asteroid, the most common spectral type among the Jupiter trojans, with few dozens already identified in the early Tholen and SMASS classification (Bus–Binzel). Priamus has also been characterized as a D-type by Pan-STARRS survey. Rotation period Several rotational lightcurves have been obtained from photometric observations since the 1980s, when Priamus was first observed by William Hartmann (1988) and Stefano Mottola (1993). The best rated result from July 2010, by Robert Stephens at GMARS and Linda French at Illinois Wesleyan University using the 0.9-meter SMARTS telescope at CTIO in Chile, gave a well-defined rotation period of hours with a consolidated brightness variation between 0.23 and 0.40 in magnitude (). In January 1993 and October 2001, two lightcurves were obtained by Stefano Mottola in collaboration with Claes-Ingvar Lagerkvist and Marco Delbo at Kvistaberg and Pino Torinese observatories, respectively (). Another measurement was made by Ukrainian astronomers in August 2010 (). Between January 2015, and December 2016, photometric observations by Robert Stephens and Daniel Coley in collaboration with Brian Warner at the Center for Solar System Studies, California, gave a three concurring periods of 6.854, 6.863 and 6.865 hours (). Diameter and albedo According to the surveys carried out by the Japanese Akari satellite and the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer, Priamus measures 101.09 and 119.99 kilometers in diameter and its surface has an albedo of 0.044 and 0.037, respectively. The Collaborative Asteroid Lightcurve Link assumes a standard albedo for a carbonaceous asteroid of 0.057 and calculates a diameter of 96.29 kilometers based on an absolute magnitude of 8.81. Notes References External links Asteroid Lightcurve Database (LCDB), query form (info ) Dictionary of Minor Planet Names, Google books Discovery Circumstances: Numbered Minor Planets (1)-(5000) – Minor Planet Center 000884 Discoveries by Max Wolf Named minor planets 000884 19170922

3036765

https://en.wikipedia.org/wiki/885%20Ulrike

885 Ulrike

885 Ulrike (prov. designation: or ) is an elongated Themistian asteroid from the outer regions of the asteroid belt. It was discovered on 23 September 1917, by Soviet astronomer Sergey Belyavsky at the Simeiz Observatory on the Crimean peninsula. The presumed C-type asteroid has a short rotation period of 4.9 hours and measures approximately in diameter. It was likely named after Ulrike von Levetzow, last love of Goethe. Orbit and classification When applying the synthetic hierarchical clustering method (HCM) by Zappalà, Milani and Knežević (AstDys), Ulrike is a core member of the Themis family (), a large asteroid family of carbonaceous asteroids named after 24 Themis. However, according to another HCM-analysis by Nesvorný, it is a background asteroid. It orbits the Sun in the outer main-belt at a distance of 2.5–3.7 AU once every 5 years and 5 months (1,992 days; semi-major axis of 3.1 AU). Its orbit has an eccentricity of 0.19 and an inclination of 3° with respect to the ecliptic. The asteroid was first observed at Lowell Observatory in August 1906. The body's observation arc begins at Heidelberg Observatory on 27 September 1906, more than a decade prior to its official discovery observation at Simeiz. Naming This minor planet was allegedly named after Ulrike von Levetzow (1804–1899), a friend and last love of the German poet Johann Wolfgang von Goethe, who met Ulrike during summertime 1821–1823 in Marienbad, Bohemia. After she declined to marry him, Goethe started writing Marienbad Elegy, one of his finest poems. Lutz Schmadel, the author of the Dictionary of Minor Planet Names, considers this interpretation the most likely because the discoverer, who studied at Göttingen University, was an expert in German literature. Physical characteristics Ulrike spectral type is unknown. It is an assumed carbonaceous C-type asteroid, which agrees with the overall spectral type assigned to members of the Themis family. Rotation period In September 2010, a rotational lightcurve of Ulrike was obtained from photometric observations by John Menke at the Menke Observatory. Lightcurve analysis gave a rotation period of hours with a high brightness variation of magnitude, indicative of an elongated shape (). An alternative period determination of hours with an even higher amplitude of was made by Laurent Bernasconi one month later in October 2010 (). A modeled lightcurve using photometric data from the Lowell Photometric Database gave a sidereal period of and two spin axes at (13.0°, −64.0°) and (207.0°, −60.0°) in ecliptic coordinates (λ, β). Diameter and albedo According to the survey carried out by the Infrared Astronomical Satellite IRAS, the Japanese Akari satellite, and the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer (WISE), Ulrike measures (), () and () kilometers in diameter and its surface has an albedo of (), () and (), respectively. The Collaborative Asteroid Lightcurve Link adopts the results from IRAS, that is an albedo of 0.083 and a diameter of 33.43 kilometers based on an absolute magnitude of 10.7. The WISE team also published an alternative mean-diameter of () with an albedo of (). References External links Lightcurve Database Query (LCDB), at www.minorplanet.info Dictionary of Minor Planet Names, Google books Asteroids and comets rotation curves, CdR – Geneva Observatory, Raoul Behrend Discovery Circumstances: Numbered Minor Planets (1)-(5000) – Minor Planet Center 000885 000885 Discoveries by Sergei Belyavsky Named minor planets Giuseppe Verdi 19170923

3036766

https://en.wikipedia.org/wiki/886%20Washingtonia

886 Washingtonia

886 Washingtonia is a minor planet orbiting the Sun. It was discovered on 16 November 1917, from Washington, D.C., and is named after the 1st President of the United States, George Washington. Discovery circumstances Credit for the discovery of 886 Washingtonia has been given to George Peters of the US Naval Observatory, who was the first to report it. The object was, however, observed four days earlier by Margaret Harwood, who was advised not to report it as a new discovery because "it was inappropriate that a woman should be thrust into the limelight with such a claim". The first woman to be credited with the discovery of a minor planet was Pelageya Fedorovna Shajn, eleven years later. References External links Lightcurve plot of 886 Washingtonia, Palmer Divide Observatory, B. D. Warner (2003) Asteroid Lightcurve Database (LCDB), query form (info ) Dictionary of Minor Planet Names, Google books Asteroids and comets rotation curves, CdR – Observatoire de Genève, Raoul Behrend Discovery Circumstances: Numbered Minor Planets (1)-(5000) – Minor Planet Center 000886 Discoveries by George Peters Named minor planets 000886 19171116

3036770

https://en.wikipedia.org/wiki/887%20Alinda

887 Alinda

887 Alinda () is a very eccentric, near-Earth asteroid with an Earth minimum orbit intersection distance (MOID) of 0.092 AU. It is the namesake for the Alinda group of asteroids and measures about 4 kilometers in diameter. The stony S-type asteroid was discovered by German astronomer Max Wolf at Heidelberg Observatory on 3 January 1918. Due to its high eccentricity and semi-major axis of 0.57 and 2.5 AU, respectively, it is a typical Amor III asteroid. It has both, a 1:3 orbital resonance with Jupiter and a close to 4:1 resonance with Earth. As a result of the resonance with Jupiter that has excited the eccentricity of the orbit over the eons, the asteroid's orbit has evolved to spend time outside of the main-belt. It is the namesake for the Alinda group of asteroids. Alinda makes close approaches to Earth, including a pass in January 2025, where it comes within of Earth. The asteroid's name had been proposed by H. Kobol. It is uncertain whether it refers to the ancient city of Alinda in modern western Turkey, or to a mythological figure of the Australian aboriginals. References External links 000887 000887 Discoveries by Max Wolf Named minor planets 000887 19180103

3036771

https://en.wikipedia.org/wiki/888%20Parysatis

888 Parysatis

888 Parysatis (prov. designation: or ) is a stony background asteroid, approximately in diameter, that is located in the central region of the asteroid belt. It was discovered by German astronomer Max Wolf at the Heidelberg Observatory on 2 February 1918. The S-type asteroid has a rotation period of 5.9 hours. It was named after the Persian Queen Parysatis from the Achaemenid Empire of the 5th century BC. Orbit and classification Located in or near the region of the Eunomia family, Parysatis is a non-family asteroid of the main belt's background population when applying the hierarchical clustering method to its proper orbital elements. It orbits the Sun in the central asteroid belt at a distance of 2.2–3.2 AU once every 4 years and 6 months (1,629 days; semi-major axis of 2.71 AU). Its orbit has an eccentricity of 0.19 and an inclination of 14° with respect to the ecliptic. The body's observation arc begins at Vienna Observatory on 24 May 1906, almost 12 years prior to its official discovery observation at Heidelberg on 2 February 1918. Naming This minor planet was named after the Persian Queen Parysatis of the Achaemenid Empire in the 5th century BC. She was the wife of the king Darius II, and the mother of Artaxerxes II of Persia, after whom the asteroid 831 Stateira was named. The was also mentioned in The Names of the Minor Planets by Paul Herget in 1955 (). Physical characteristics In the Tholen classification, Parysatis is a common stony S-type asteroid. Rotation period In November 2006, a rotational lightcurve of Parysatis was obtained from photometric observations by Serbian astronomer Vladimir Benishek at Belgrade Observatory. Lightcurve analysis gave a well-defined rotation period of hours with a brightness variation of magnitude (). The result supersedes other period determinations of () by Marcos Florczak in 1996, () by Laurent Bernasconi in 2003, and () by Michael Fleenor in 2006, and by Andy Monson in 2011 (). In April 2017, another lightcurve with a well-defined period of hours and an amplitude of magnitude was obtained by the Spanish group of asteroid observers, OBAS (). Diameter and albedo According to the survey carried out by the Japanese Akari satellite, the Infrared Astronomical Satellite IRAS, and the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer (WISE), Parysatis measures (), () and () kilometers in diameter and its surface has an albedo of (), () and (), respectively. The Collaborative Asteroid Lightcurve Link adopts the results obtained by IRAS, that is, an albedo of 0.1392 and a diameter of 44.65 kilometers with an absolute magnitude of 9.51. Alternative mean-diameter measurements published by the WISE team include (), () and () with corresponding albedos of (), () and (). References External links Lightcurve Database Query (LCDB), at www.minorplanet.info Dictionary of Minor Planet Names, Google books Asteroids and comets rotation curves, CdR – Geneva Observatory, Raoul Behrend Discovery Circumstances: Numbered Minor Planets (1)-(5000) – Minor Planet Center 000888 Discoveries by Max Wolf Named minor planets 000888 19180202

3036777

https://en.wikipedia.org/wiki/890%20Waltraut

890 Waltraut

890 Waltraut is an Eoan asteroid from the outer region of the asteroid belt that was discovered by German astronomer Max Wolf on 11 March 1918. It was named for a character in Richard Wagner's opera, Götterdämmerung (Twilight of the Gods). This is a member of the dynamic Eos family of asteroids that most likely formed as the result of a collisional breakup of a parent body. References External links 000890 Discoveries by Max Wolf Named minor planets 000890 19180311

3036778

https://en.wikipedia.org/wiki/889%20Erynia

889 Erynia

889 Erynia is a highly elongated background asteroid from the inner regions of the asteroid belt. It was discovered on 5 March 1918, by German astronomer Max Wolf at the Heidelberg-Königstuhl State Observatory, and given the provisional designations and . The stony S-type asteroid (Sl) has a rotation period of 9.89 hours and measures approximately in diameter. It was named from Greek mythology, after the Erinyes, also known as Furies. Orbit and classification Erynia is a non-family asteroid of the main belt's background population when applying the hierarchical clustering method to its proper orbital elements. It orbits the Sun in the inner asteroid belt at a distance of 2.0–2.9 AU once every 3 years and 10 months (1,398 days; semi-major axis of 2.45 AU). Its orbit has an eccentricity of 0.20 and an inclination of 8° with respect to the ecliptic. The asteroid was first observed as () at the Johannesburg Observatory on 7 August 1912. The body's observation arc begins at Heidelberg Observatory on 16 March 1918, or eleven nights after its official discovery observation. Naming This minor planet was named after one of the Erinyes from Greek mythology, also known as Furies in Roman mythology. The female deities of vengeance have snakes for hair, dog's heads, coal black bodies, bat's wings, and blood-shot eyes. They tortured their victims with brass-studded scourges and inflicted plagues. The was mentioned in The Names of the Minor Planets by Paul Herget in 1955 (). Physical characteristics In the Tholen-like taxonomy of the Small Solar System Objects Spectroscopic Survey (S3OS2), Erynia is a common stony S-type asteroid, while in the SMASS-like taxonomic variant of the survey, it is an Sl-subtype, which transitions from the S- to the uncommon L-type. Rotation period and poles In January 2002, a rotational lightcurve of Erynia was obtained from photometric observations by French astronomer Laurent Bernasconi. Lightcurve analysis gave a rotation period of hours with a high brightness variation of magnitude, indicative of a non-spherical, elongated shape (). A concurring period of hours and an amplitude 0.47 magnitude was obtained by astronomers at the Palomar Transient Factory in April 2010 (). In 2011, a modeled lightcurve using data from the Uppsala Asteroid Photometric Catalogue (UAPC) and other sources gave a sidereal period hours, as well as two spin axes at (187.0°, −60.0°) and (335.0°, −74.0°) in ecliptic coordinates (λ, β). Diameter and albedo According to the survey carried out by the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer (WISE) and the Japanese Akari satellite, Erynia measures () and () kilometers in diameter and its surface has an albedo of () and (), respectively. The Collaborative Asteroid Lightcurve Link assumes a standard albedo for a stony asteroid of 0.20 and calculates a diameter of 18.75 kilometers based on an absolute magnitude of 11.The WISE team also published a mean-diameter of () with a corresponding albedo of (). References External links Lightcurve Database Query (LCDB), at www.minorplanet.info Dictionary of Minor Planet Names, Google books Asteroids and comets rotation curves, CdR – Geneva Observatory, Raoul Behrend Discovery Circumstances: Numbered Minor Planets (1)-(5000) – Minor Planet Center 000889 Discoveries by Max Wolf Named minor planets 19180305

3036779

https://en.wikipedia.org/wiki/891%20Gunhild

891 Gunhild

891 Gunhild (prov. designation: or ) is a large background asteroid from the outer regions of the asteroid belt, that measures approximately in diameter. It was discovered on 17 May 1918, by astronomer Max Wolf at the Heidelberg-Königstuhl State Observatory in southwest Germany. The dark D-type asteroid has a rotation period of 11.9 hours. Any reference of the asteroid's name to a person is unknown. Orbit and classification Gunhild is a non-family asteroid of the main belt's background population when applying the hierarchical clustering method to its proper orbital elements. It orbits the Sun in the outer asteroid belt at a distance of 2.8–2.9 AU once every 4 years and 10 months (1,769 days; semi-major axis of 2.86 AU). Its orbit has an eccentricity of 0.03 and an inclination of 14° with respect to the ecliptic. The asteroid was first observed as () at Simeiz Observatory in November 1915. The body's observation arc begins at Heidelberg Observatory on 18 May 1918, the night after its official discovery observation. Naming This minor planet is named after a Feminine German first name. Any reference of this name to a person or occurrence is unknown. Unknown meaning Among the many thousands of named minor planets, Gunhild is one of 120 asteroids, for which no official naming citation has been published. All of these low-numbered asteroids have numbers between and and were discovered between 1876 and the 1930s, predominantly by astronomers Auguste Charlois, Johann Palisa, Max Wolf and Karl Reinmuth. Physical characteristics In both the Tholen- and SMASS-like taxonomy of the Small Solar System Objects Spectroscopic Survey (S3OS2), as well as in the SDSS-based taxonomy, Gunhild is a dark D-type asteroid. This asteroid spectral type is common among outer belt asteroids and very common among the Jupiter trojan population. Rotation period In July 2015, a rotational lightcurve of Gunhild was obtained from photometric observations by the Spanish group of asteroid observers, OBAS. Lightcurve analysis gave a rotation period of hours with a brightness amplitude of magnitude (). The result supersedes period determinations of () by Robert Stephens in 2000, () by Laurent Bernasconi in 2005, and () by Janus Kozdon in 2015 (). Diameter and albedo According to the survey carried out by the Infrared Astronomical Satellite IRAS, the Japanese Akari satellite, and the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer (WISE), Gunhild measures (), () and () kilometers in diameter and its surface has an albedo of (), () and (), respectively. The Collaborative Asteroid Lightcurve Link derives an albedo of 0.0656 and a diameter of 51.89 kilometers based on an absolute magnitude of 10.0. Alternative mean-diameter measurements published by the WISE team include (), () and () with corresponding albedos of (), () and (). Several asteroid occultation observed between 2010 and 2014 gave a best-fit ellipse dimension of 52.0 × 52.0 kilometers (one observation) and 63.0 × 63.0 kilometers (three observations). These timed observations are taken when the asteroid passes in front of a distant star. References External links Lightcurve Database Query (LCDB), at www.minorplanet.info Dictionary of Minor Planet Names, Google books Asteroids and comets rotation curves, CdR – Geneva Observatory, Raoul Behrend Discovery Circumstances: Numbered Minor Planets (1)-(5000) – Minor Planet Center 000891 Discoveries by Max Wolf Named minor planets 19180517

3036780

https://en.wikipedia.org/wiki/892%20Seeligeria

892 Seeligeria

892 Seeligeria is dark Alauda asteroid from the outer region of the asteroid belt that was discovered by German astronomer Max Wolf on May 31, 1918 in Heidelberg and assigned a preliminary designation of 1918 DR. It was named after German astronomer Hugo Hans von Seeliger. Photometric observations at the Oakley Observatory in Terre Haute, Indiana, during 2007 were used to build a light curve for 892 Seeligeria. The asteroid displayed a rotation period of 15.78 ± 0.04 hours and a brightness variation of 0.35 ± 0.07 in magnitude. Seeligeria is a member of the Alauda family (), a large family of typically bright carbonaceous asteroids and named after its parent body, 702 Alauda. References External links 000892 Discoveries by Max Wolf Named minor planets 19180531

3036782

https://en.wikipedia.org/wiki/893%20Leopoldina

893 Leopoldina

893 Leopoldina (prov. designation: or ) is a large and elongated background asteroid from the outer regions of the asteroid belt. It was discovered by German astronomer Max Wolf at the Heidelberg Observatory on 31 May 1918. The dark carbonaceous C-type asteroid has a rotation period of 14.1 hours and measures approximately in diameter. It was named for Germany's national academy, the Academy of Sciences Leopoldina in Halle. Orbit and classification Leopoldina is a non-family asteroid of the main belt's background population when applying the hierarchical clustering method to its proper orbital elements. It orbits the Sun in the outer asteroid belt at a distance of 2.6–3.5 AU once every 5 years and 4 months (1,950 days; semi-major axis of 3.05 AU). Its orbit has an eccentricity of 0.15 and an inclination of 17° with respect to the ecliptic. The body's observation arc begins with its official discovery observation at Heidelberg Observatory on 31 May 1918. Physical characteristics In the Tholen classification, Leopoldinas asteroid spectral type is closest to that of an X-type, and somewhat similar to that of a dark F-type asteroid (XF), while in both the Tholen- and SMASS-like taxonomy of the Small Solar System Objects Spectroscopic Survey (S3OS2), it is a common carbonaceous C-type asteroid. Naming This minor planet was named for Germany's national academy, the Academy of Sciences Leopoldina () in Halle, Saxony-Anhalt. The was mentioned in The Names of the Minor Planets by Paul Herget in 1955 (). Rotation period In April 2008, a rotational lightcurve of Leopoldina was obtained from photometric observations by Brian Warner at the Palmer Divide Observatory in Colorado. Analysis gave a classically shaped bimodal lightcurve with a well-defined rotation period of hours and a brightness variation of magnitude (). The result supersedes Warner's previous observation from August 2005, which determined a period of hours and an amplitude of magnitude (). Diameter and albedo According to the survey carried out by the Japanese Akari satellite, the Infrared Astronomical Satellite IRAS, and the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer (WISE), Leopoldina measures (), () and () kilometers in diameter and its surface has an albedo of (), () and (), respectively. The Collaborative Asteroid Lightcurve Link adopts the results obtained by IRAS, that is, an albedo of 0.0497 and a diameter of 76.14 kilometers based on an absolute magnitude of 9.47. Alternative mean-diameter measurements published by the WISE team include (), (), (), () and () with albedos in the range of 0.049 to 0.06. Three asteroid occultation were obtained on 29 January 1996, 30 August 2010 and 16 May 2015. They gave a best-fit ellipse dimension of 79.0 × 72.0 kilometers, 82.8 × 59.8 kilometers (best), and 75.0 × 75.0 kilometers, respectively. These timed observations are taken when the asteroid passes in front of a distant star. Notes References External links Lightcurve Database Query (LCDB), at www.minorplanet.info Dictionary of Minor Planet Names, Google books Discovery Circumstances: Numbered Minor Planets (1)-(5000) – Minor Planet Center 000893 Discoveries by Max Wolf Named minor planets 000893 19180531

3036784

https://en.wikipedia.org/wiki/894%20Erda

894 Erda

894 Erda (prov. designation: or ) is a bright background asteroid from the outer regions of the asteroid belt. It was discovered on 4 June 1918, by German astronomer Max Wolf at the Heidelberg-Königstuhl State Observatory. The X-type asteroid has a short rotation period of 4.7 hours and measures approximately in diameter. It was likely named after a character in Wagner's Der Ring des Nibelungen, "Erda", who is the goddess of wisdom, fate and Earth, borrowed from the Norse sagas, and referring to both Urðr and Jörð in Norse mythology. Orbit and classification Erda is a non-family asteroid of the main belt's background population when applying the hierarchical clustering method to its proper orbital elements. It orbits the Sun in the outer main-belt at a distance of 2.8–3.5 AU once every 5 years and 6 months (2,013 days; semi-major axis of 3.12 AU). Its orbit has an eccentricity of 0.11 and an inclination of 13° with respect to the ecliptic. On 14 May 1907, the body's observation arc begins as () at Heidelberg; just two nights after its first observation, and more than 11 years prior to its official discovery observation. Naming According to The Names of the Minor Planets by Paul Herget in 1955, and adopted by Lutz Schmadel in the Dictionary of Minor Planet Names, this minor planet was named after the Norse goddess described as the "incarnation of the nature", and as "a seer who knows the origin and the destination of all things" (). The discoverer, Max Wolf, likely adopted the name from Wagner's opera cycle Der Ring des Nibelungen, which is loosely based on figures from the Norse sagas. In Wagner's Ring, the character , named after the Old High German word for "Earth", is the goddess of wisdom, fate and Earth. She is the world's wisest woman, the mother of the three Norns and of the valkyrie (shieldmaid) Brunhild, whose father is the norse chief god Odin (Wotan). Wagner, in turn, adopted the name from the treatise Deutsche Mythologie by Jacob Grimm (1785–1863) and other sources. Erda combines attributes of both, Urðr (wisdom and fate) and Jörð (the personification of Earth). Physical characteristics In both the Tholen- and SMASS-like taxonomy of the Small Solar System Objects Spectroscopic Survey (S3OS2), Erda is an X-type asteroid. Rotation period In June 2006, a rotational lightcurve of Erda was obtained from photometric observations by David Higgins at Hunters Hill Observatory , Australia, and by Rui Gonçalves at Linhaceira Observatory in Portugal. Lightcurve analysis gave a well-defined rotation period of hours with a brightness variation of magnitude, significantly higher than previous observations had measured (). The observers also found no indication of a previously speculated companion. The result supersedes observations from July 2001, when both Robert Stephens and Laurent Bernasconi determined a period of and hours with an amplitude of and magnitude, respectively. Diameter and albedo According to the survey carried out by the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer (WISE), the Infrared Astronomical Satellite IRAS, and the Japanese Akari satellite, Erda measures (), () and () kilometers in diameter and its surface has an albedo of (), () and (), respectively. The Collaborative Asteroid Lightcurve Link derives an albedo of 0.1942 and a diameter of 36.26 kilometers based on an absolute magnitude of 9.6. An alternative mean-diameter measurement published by the WISE team gives () with an albedo of (). On 17 April 2010, an asteroid occultation gave a best-fit ellipse dimension of 36.00 × 36.0 kilometers, while a second observation on 15 September 2014, measured an ellipse of 38.00 × 38.0 kilometers These timed observations are taken when the asteroid passes in front of a distant star. References External links Lightcurve Database Query (LCDB), at www.minorplanet.info Dictionary of Minor Planet Names, Google books Asteroids and comets rotation curves, CdR – Geneva Observatory, Raoul Behrend Discovery Circumstances: Numbered Minor Planets (1)-(5000) – Minor Planet Center 000894 Discoveries by Max Wolf Named minor planets 19180604

3036785

https://en.wikipedia.org/wiki/895%20Helio

895 Helio

895 Helio is a large dark outer main-belt asteroid about 150 km in diameter. It was discovered on 11 July 1918 by German astronomer Max Wolf. It is named after the element helium, whose spectrum was studied by Friedrich Paschen and Carl David Tolmé Runge, with the asteroid being named by Paschen at Wolf's request; the name helium itself comes from Helios, the Greek god of the Sun. This is a B-type asteroid. The best spectral analog for 895 Heloi is the iron rich pyroxene mineral hedenbergite. It shares similar orbital properties with the 31 Euphrosyne asteroid family, but is most likely an interloper. Light curve analysis provides a rotation period of 9.4 hours. References External links 000895 Discoveries by Max Wolf Named minor planets 000895 000895 19180711

3036787

https://en.wikipedia.org/wiki/896%20Sphinx

896 Sphinx

896 Sphinx is a background asteroid from the inner regions of the asteroid belt, that measures approximately in diameter. It was discovered on 1 August 1918, by astronomer Max Wolf at the Heidelberg-Königstuhl State Observatory in southwest Germany. The asteroid has a rotation period of 21.0 hours and is one of few low-numbered objects for which no spectral type has been determined. It was named after the Sphinx, a creature from Greek and Egyptian mythology. Orbit and classification Sphinx is a non-family asteroid of the main belt's background population when applying the hierarchical clustering method to its proper orbital elements. It orbits the Sun in the inner asteroid belt at a distance of 1.9–2.7 AU once every 3 years and 6 months (1,262 days; semi-major axis of 2.29 AU). Its orbit has an eccentricity of 0.16 and an inclination of 8° with respect to the ecliptic. The body's observation arc begins at Heidelberg Observatory on 9 October 1918, two months after its official discovery observation. Naming This minor planet was named after the Sphinx, a legendary creature from Greek and Egyptian mythology. The female monster has the head of a woman, the haunches of a lion, and the wings of a bird. It has the habit of killing anyone who cannot answer her riddle. The was mentioned in The Names of the Minor Planets by Paul Herget in 1955 (). Physical characteristics Contrary to most other low-numbered asteroids, no spectral type has been determined. Based on its relatively high albedo (see below) and its location within the inner parts of the main-belt, Sphinx may possibly be a common, stony S-type asteroid. Rotation period In June 2018, a rotational lightcurve of Sphinx was obtained from photometric observations by Tom Polakis at the Command Module Observatory in Arizona. Lightcurve analysis gave a rotation period of hours with a brightness variation of magnitude (). However, an alternative period solution of hours with an amplitude of magnitude is also possible. Both results supersede a tentative period determination by Laurent Bernasconi from September 2001 (). A modeled lightcurve using photometric data from the Lowell Photometric Database and from the Wide-field Infrared Survey Explorer (WISE) was published in 2018. It gave a divergent sidereal period of hours and includes two spin axes at (172.0°, 20.0°) and (352.0°, 42.0°) in ecliptic coordinates (λ, β). Diameter and albedo According to the surveys carried out by the NEOWISE mission of NASA's WISE telescope, the Infrared Astronomical Satellite IRAS, and the Japanese Akari satellite, Sphinx measures (), () and () kilometers in diameter and its surface has an albedo of (), () and (), respectively. The Collaborative Asteroid Lightcurve Link derives an albedo of 0.2332 and a diameter of 13.17 kilometers based on an absolute magnitude of 11.6. Alternative mean-diameter measurements published by the WISE team include (), () and () with corresponding albedos of (), () and (). References External links Lightcurve Database Query (LCDB), at www.minorplanet.info Dictionary of Minor Planet Names, Google books Asteroids and comets rotation curves, CdR – Geneva Observatory, Raoul Behrend Discovery Circumstances: Numbered Minor Planets (1)-(5000) – Minor Planet Center 000896 Discoveries by Max Wolf Named minor planets 19180801 Sphinxes

3036788

https://en.wikipedia.org/wiki/897%20Lysistrata

897 Lysistrata

897 Lysistrata is a minor planet orbiting the Sun that was discovered by German astronomer Max Wolf on August 3, 1918. This is a member of the dynamic Maria family of asteroids that most likely formed as the result of a collisional breakup of a parent body. References External links 000897 Discoveries by Max Wolf Named minor planets Aristophanes 000897 000897 19180803

3036789

https://en.wikipedia.org/wiki/898%20Hildegard

898 Hildegard

898 Hildegard is a bright background asteroid, approximately in diameter, that is located in the central regions of the asteroid belt. It was discovered by German astronomer Max Wolf at the Heidelberg-Königstuhl State Observatory on 3 August 1918 and given the provisional designations and . The stony S-type asteroid (Sl) has a rotation period of 24.9 hours and a relatively high orbital eccentricity of 0.37. It was probably named after Saint Hildegard of Bingen (1098–1179). Orbit and classification Hildegard is a non-family asteroid of the main belt's background population when applying the hierarchical clustering method to its proper orbital elements. It orbits the Sun in the central asteroid belt at a distance of 1.7–3.7 AU once every 4 years and 6 months (1,648 days; semi-major axis of 2.73 AU). Its orbit has a high eccentricity of 0.37 and an inclination of 10° with respect to the ecliptic. With a perihelion of 1.72 AU, Hildegard is notably close of becoming an outer-grazer to Mars, which has its aphelion at 1.67 AU. The body's observation arc begins at Heidelberg Observatory with its official discovery observation on 3 August 1918. Naming This minor planet was probably named after Saint Hildegard of Bingen (1098–1179). The Benedictine abbess is considered to be the founder of scientific natural history in Germany. The was also mentioned in The Names of the Minor Planets by Paul Herget in 1955 (). Physical characteristics In the Bus–Binzel SMASS classification, Hildegard is an Sl-subtype, which transitions from the common stony S-type to the uncommon L-type asteroid. Rotation period In April 2008, a rotational lightcurve of Hildegard was obtained from photometric observations by Australian amateur astronomer David Higgins. Lightcurve analysis gave a well-defined rotation period of hours with a brightness variation of magnitude (). Previously in June 1999, observations by Brian Warner at his Palmer Divide Observatory in Colorado only gave a period of above 24 hours and an amplitude larger than 0.3 magnitude (). Asteroid's with a rotation period near 24 hours are difficult to observe, since full coverage can not be obtained by a few consecutive nights of observation from a single observatory alone, due to Earth's nearly synchronous rotation. In such cases, international collaborations are highly useful with each observatory covering a different section of the lightcurve. In 2016, a modeled lightcurve gave a concurring sidereal period of hours using data from a large collaboration of individual observers (such as above). The study also determined two spin axes of (344.0°, 27.0°) and (164.0°, 8.0°) in ecliptic coordinates (λ, β). Diameter and albedo According to the survey carried out by the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer, Hildegard measures kilometers in diameter and its surface has an albedo of . The Collaborative Asteroid Lightcurve Link assumes a standard albedo for a stony asteroid of 0.20 and calculates a diameter of 13.58 kilometers based on an absolute magnitude of 11.7. Notes References External links Lightcurve Database Query (LCDB), at www.minorplanet.info Dictionary of Minor Planet Names, Google books Discovery Circumstances: Numbered Minor Planets (1)-(5000) – Minor Planet Center 000898 Discoveries by Max Wolf Named minor planets 898 Hildegard 000898 19180803

3036790

https://en.wikipedia.org/wiki/899%20Jokaste

899 Jokaste

899 Jokaste is a minor planet orbiting the Sun. It was one of five minor planets included in the 1993 study, Transition Comets -- UV Search for OH Emissions in Asteroids, which was research involving amateur astronomers who were permitted to make use of the Hubble Space Telescope. Not to be confused with Iocaste, a moon of Jupiter. References External links 000899 Discoveries by Max Wolf Named minor planets 000899 19180803

3036792

https://en.wikipedia.org/wiki/900%20Rosalinde

900 Rosalinde

900 Rosalinde (prov. designation: or ) is an elongated background asteroid from the inner regions of the asteroid belt, that has a mean-diameter of approximately . It was discovered on 10 August 1918, by astronomer Max Wolf at the Heidelberg-Königstuhl State Observatory in southwest Germany. The lengthy S/D-type asteroid has a rotation period of 16.6 hours. It was likely named after "Rosalinde", a character in the operetta Die Fledermaus by Johann Strauss II. Orbit and classification Rosalinde is a non-family asteroid of the main belt's background population when applying the hierarchical clustering method to its proper orbital elements. It orbits the Sun in the inner asteroid belt at a distance of 2.1–2.9 AU once every 3 years and 11 months (1,421 days; semi-major axis of 2.47 AU). Its orbit has an eccentricity of 0.16 and an inclination of 12° with respect to the ecliptic. The body's observation arc begins at Heidelberg-Königstuhl State Observatory with its official discovery observation on 10 August 1918. Naming This minor planet was probably named after the character "Rosalinde", Eisenstein's wife, in the operetta Die Fledermaus by Johann Strauss II (1825–1899), after whom 4559 Strauss was named. Rosalinde's maid in the operetta, "Adele", is likely the namesake chosen by Wolf for another asteroid, 812 Adele. Lutz Schmadel, the author of the Dictionary of Minor Planet Names learned about the discoverer's source of inspiration from private communications with Dutch astronomer Ingrid van Houten-Groeneveld, who worked as a young astronomer at the discovering Heidelberg Observatory. Physical characteristics Rosalinde is an S-type/D-type in the SMASS-I spectral type-classification by Xu (1995), which surveyed and classified a total of 221 objects. However, Rosalindes classification, with its moderate albedo of 0.1 (see below) does not correspond to more modern taxonomies such as the Bus–Binzel SMASS classification (II), where the bright S-types and the dark D-types do not have intermediate albedos. Rotation period In June 2011, a rotational lightcurve of Rosalinde was obtained from photometric observations by Meaghann Stoelting and David DeGraffat at the Stull Observatory of the Alfred University in New York. Lightcurve analysis gave a rotation period of hours with a brightness variation of magnitude (). Assuming an equatorial view, the observers also constrained the object's elongated shape to be at least 36% longer than wide. The result supersedes a tentative period determination by French amateur astronomer René Roy from May 2007 (). Additional observation by the Spanish OBAS group gave a period of hours with an amplitude of magnitude (). In 2016, a modeled lightcurve gave a concurring sidereal period of hours using data from the Uppsala Asteroid Photometric Catalogue, the Palomar Transient Factory survey, and individual observers (such as above), as well as sparse-in-time photometry from the NOFS, the Catalina Sky Survey, and the La Palma surveys . The study also determined two spin axes of (276.0°, 70.0°) and (90.0°, 39.0°) in ecliptic coordinates (λ, β). Diameter and albedo According to the survey carried out by the Infrared Astronomical Satellite IRAS, the Japanese Akari satellite, and the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer (WISE), Rosalinde measures (), () and () kilometers in diameter and its surface has an albedo of (), () and (), respectively. The Collaborative Asteroid Lightcurve Link assumes an albedo of 0.0931 and calculates a diameter of 18.75 kilometers based on an absolute magnitude of 11.83. Alternative mean-diameter measurements published by the WISE team include (), () and () with corresponding albedos of (), () and (). On 7 June 2015, an asteroid occultation gave a best-fit ellipse dimension of 19.0 × 19.0 kilometers. These timed observations are taken when the asteroid passes in front of a distant star. References External links Lightcurve Database Query (LCDB), at www.minorplanet.info Dictionary of Minor Planet Names, Google books Asteroids and comets rotation curves, CdR – Geneva Observatory, Raoul Behrend Discovery Circumstances: Numbered Minor Planets (1)-(5000) – Minor Planet Center 000900 Discoveries by Max Wolf Named minor planets Johann Strauss II 19180810

3036795

https://en.wikipedia.org/wiki/812%20Adele

812 Adele

812 Adele (prov. designation: or ) is an elongated Eunomia asteroid from the central regions of the asteroid belt. It was discovered on 8 September 1915, by Russian astronomer Sergey Belyavsky at the Simeiz Observatory on the Crimean peninsula. The presumed S-type asteroid has a rotation period of 5.9 hours and measures approximately in diameter. It was likely named after the character "Adele" in the opera Die Fledermaus by Johann Strauss. Orbit and classification When applying the hierarchical clustering method to its proper orbital elements, Adele is a core member of the Eunomia family (), a prominent family of stony S-type asteroids and the largest one in the intermediate main belt with more than 5,000 known members. It orbits the Sun in the central asteroid belt at a distance of 2.2–3.1 AU once every 4 years and 4 months (1,585 days; semi-major axis of 2.66 AU). Its orbit has an eccentricity of 0.16 and an inclination of 13° with respect to the ecliptic. Discovery Adele was discovered by Russian astronomer Sergey Belyavsky at the Simeiz Observatory on the Crimean peninsula 8 September 1915. Three nights later, on 11 September 1915, it was independently discovered by Max Wolf the Heidelberg Observatory in Germany. The Minor Planet Center however, only credits the first discoverer. The asteroid was first observed as at Heidelberg on 25 October 1902. The body's observation arc begins at the Bergedorf Observatory on 19 September 1915, less than two weeks after its official discovery observation. Naming This minor planet was likely named after "Adele", Rosalinde's maid, a character in the operetta Die Fledermaus by Johann Strauss (1825–1899). The name was given by the independent discoverer Max Wolf. The author of the Dictionary of Minor Planet Names, Lutz Schmadel, learned about the meaning of the asteroid's name from R. Bremer and Ingrid van Houten-Groeneveld, latter who worked as a young astronomer at Heidelberg. Physical characteristics Based on the overall spectral type of the Eunomia family, Adele is likely a common, stony S-type asteroid. Rotation period In October 2002, a rotational lightcurve of Adele was obtained from photometric observations by French amateur astronomer René Roy. Lightcurve analysis gave a well-defined rotation period of hours with a high brightness variation of magnitude, indicative of an elongated shape (). In 2016, a modeled lightcurve gave a concurring sidereal period of hours using data from the Uppsala Asteroid Photometric Catalogue, the Palomar Transient Factory survey, and individual observers (such as above), as well as sparse-in-time photometry from the NOFS, the Catalina Sky Survey, and the La Palma surveys . The study also determined two spin axes at (301.0°, 44.0°) and (154.0°, 69.0°) in ecliptic coordinates (λ, β). Diameter and albedo According to the surveys carried out by the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer (WISE) and the Japanese Akari satellite, Adele measures () and () kilometers in diameter and its surface has an albedo of () and (), respectively. The Collaborative Asteroid Lightcurve Link assumes a standard albedo for a Eunomian asteroid of 0.21 and calculates a diameter of 12.66 kilometers based on an absolute magnitude of 11.8. Alternative mean-diameter measurements published by the WISE team include () and () with corresponding albedos of () and (). References External links Lightcurve Database Query (LCDB), at www.minorplanet.info Dictionary of Minor Planet Names, Google books Asteroids and comets rotation curves, CdR – Geneva Observatory, Raoul Behrend Discovery Circumstances: Numbered Minor Planets (1)-(5000) – Minor Planet Center 000812 Discoveries by Sergei Belyavsky 19150908

3036797

https://en.wikipedia.org/wiki/824%20Anastasia

824 Anastasia

824 Anastasia is a main belt asteroid orbiting the Sun. It is approximately 34.14 km in diameter. It was discovered on March 25, 1916, by Grigory Neujmin at Simeiz Observatory in Russian Empire. It is named in memory of Anastasia Semenoff, an acquaintance of the discoverer. Occultation On April 6, 2010, 824 Anastasia had the distinction of causing the brightest asteroid occultation ever predicted for North America for an asteroid of its size. The asteroid occulted the naked-eye star ζ Ophiuchi over a path stretching from the Los Angeles area to Edmonton, Alberta. References External links 000824 Discoveries by Grigory Neujmin Named minor planets 000824 000824 000824 19160325

3036798

https://en.wikipedia.org/wiki/829%20Academia

829 Academia

829 Academia is a minor planet orbiting the Sun. The asteroid is roughly 44 km in diameter and has a low albedo. Photometric measurements of the asteroid made in 2005 at the Palmer Divide Observatory showed a light curve with a period of 7.891 ± 0.005 hours and a brightness variation of 0.44 ± 0.02 in magnitude. References External links Lightcurve plot of 829 Academia, Palmer Divide Observatory, B. D. Warner (2005) Asteroid Lightcurve Database (LCDB), query form (info ) Dictionary of Minor Planet Names, Google books Asteroids and comets rotation curves, CdR – Observatoire de Genève, Raoul Behrend Discovery Circumstances: Numbered Minor Planets (1)-(5000) – Minor Planet Center 000829 Discoveries by Grigory Neujmin Named minor planets 19160825

3036819

https://en.wikipedia.org/wiki/845%20Na%C3%ABma

845 Naëma

845 Naëma (prov. designation: or ) is a large asteroid and the parent body of the Naëma family located in the outer regions of the asteroid belt. It was discovered on 16 November 1916, by astronomer Max Wolf at the Heidelberg-Königstuhl State Observatory in southwest Germany. The carbonaceous C-type asteroid has a rotation period of 20.9 hours and measures approximately in diameter on average, as it is likely elongated in shape. Any reference of the asteroid's name to a person is unknown. Orbit and classification Naëma is the parent body of the Naëma family (), a smaller family of little more than 300 carbonaceous asteroids, when applying the hierarchical clustering method. This asteroid family is widely recognized by a number of Solar System dynamicists including Zappalà, Nesvorný, as well as Milani and Knežević (AstDyS) The family was first detected by Vincenzo Zappalà in 1994/95. Naëma orbits the Sun in the outer asteroid belt at a distance of 2.7–3.1 AU once every 5.04 years (1,840 days; semi-major axis of 2.94 AU). Its orbit has an eccentricity of 0.07 and an inclination of 13° with respect to the ecliptic. The body's observation arc begins as () with its official discovery observation at Heidelberg Observatory on 16 November 1916. Naming Naëma is a German variant of the biblical name Naomi. However, any reference of this minor planet name to a person or occurrence is unknown. Unknown meaning Among the many thousands of named minor planets, Naëma is one of 120 asteroids for which no official naming citation has been published. All of these asteroids have low numbers, the first being . The last asteroid with a name of unknown meaning is . They were discovered between 1876 and the 1930s, predominantly by astronomers Auguste Charlois, Johann Palisa, Max Wolf and Karl Reinmuth. Physical characteristics In the Bus–Binzel SMASS classification, Naëma is a common, carbonaceous C-type asteroid, which is the overall spectral type of the Naëma family. Rotation period In September 2006, a rotational lightcurve of Naëma was obtained from photometric observations by Collin Bembrick at the Mount Tarana Observatory , Australia, in collaboration with Bill Allen and Greg Bolt. Lightcurve analysis gave a relatively long rotation period of hours with a brightness variation of magnitude (). In December 2017, French amateur astronomer René Roy determined a lower-rated, tentative period of hours with an amplitude of magnitude (). Diameter and albedo According to the surveys carried out by the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer (WISE), the Infrared Astronomical Satellite IRAS, and the Japanese Akari satellite, Naëma measures (), () and () kilometers in diameter and its surface has an albedo of (), () and (), respectively. The Collaborative Asteroid Lightcurve Link derives an albedo of 0.0503 and a diameter of 54.05 kilometers based on an absolute magnitude of 10.2. Alternative mean-diameter measurements published by the WISE team include (), (), (), () and () with corresponding albedos of (), (), (), () and (). Several asteroid occultations of Naëma have been observed between 2002 and 2010. The best-rated one from 10 April 2010, gave a best-fit ellipse dimension of (). These timed observations are taken when the asteroid passes in front of a distant star. References External links Lightcurve Database Query (LCDB), at www.minorplanet.info Dictionary of Minor Planet Names, Google books Asteroids and comets rotation curves, CdR – Geneva Observatory, Raoul Behrend Discovery Circumstances: Numbered Minor Planets (1)-(5000) – Minor Planet Center 000845 Discoveries by Max Wolf Named minor planets 000845 19161116

3036860

https://en.wikipedia.org/wiki/Operation%20Fishbowl

Operation Fishbowl

Operation Fishbowl was a series of high-altitude nuclear tests in 1962 that were carried out by the United States as a part of the larger Operation Dominic nuclear test program. Flight-test vehicles were designed and manufactured by Avco Corporation. Introduction The Operation Fishbowl nuclear tests were originally to be completed during the first half of 1962 with three tests named Bluegill, Starfish and Urraca. The first test attempt was delayed until June. Planning for Operation Fishbowl, as well as many other nuclear tests in the region, began rapidly in response to the sudden Soviet announcement on August 30, 1961 that they were ending a three-year moratorium on nuclear testing. The rapid planning of very complex operations necessitated many as the project progressed. All of the tests were to be launched on missiles from Johnston Island in the Pacific Ocean north of the equator. Johnston Island had already been established as a launch site for United States high-altitude nuclear tests, rather than the other locations in the Pacific Proving Grounds. In 1958, Lewis Strauss, then chairman of the United States Atomic Energy Commission, opposed doing any high-altitude tests at locations that had been used for earlier Pacific nuclear tests. His opposition was motivated by fears that the flash from the nighttime high-altitude detonations might blind civilians who were living on nearby islands. Johnston Island was a remote location, more distant from populated areas than other potential test locations. To protect residents of the Hawaiian Islands from flash blindness or permanent retinal injury from the bright nuclear flash, the nuclear missiles of Operation Fishbowl were launched generally toward the southwest of Johnston Island so that the detonations would be farther from Hawaii. Urraca was to be a test of about 1 megaton yield at very high altitude (above 1000 km.). The proposed Urraca test was always controversial, especially after the damage caused to satellites by the Starfish Prime detonation, as described below. Urraca was finally canceled, and an extensive re-evaluation of the Operation Fishbowl plan was made during an 82-day operations pause after the Bluegill Prime disaster of July 25, 1962, as described below. A test named Kingfish was added during the early stages of Operation Fishbowl planning. Two low-yield tests, Checkmate and Tightrope, were also added during the project, so the final number of tests in Operation Fishbowl was five. Tightrope was the last atmospheric nuclear test conducted by the United States, as the Limited Test Ban Treaty came into effect shortly thereafter. Research directions The United States completed six high-altitude nuclear tests in 1958, but the high-altitude tests of that year raised a number of questions. According to U.S. Government Report ADA955694 on the first successful test of the Fishbowl series, "Previous high-altitude nuclear tests: Teak, Orange, and Yucca, plus the three ARGUS shots were poorly instrumented and hastily executed. Despite thorough studies of the meager data, present models of these bursts are sketchy and tentative. These models are too uncertain to permit extrapolation to other altitudes and yields with any confidence. Thus there is a strong need, not only for better instrumentation, but for further tests covering a range of altitudes and yields." There were three phenomena in particular that required further investigation: The electromagnetic pulse generated by a high-altitude nuclear explosion appeared to have very significant differences from the electromagnetic pulse generated by nuclear explosions closer to the surface. The auroras associated with high-altitude nuclear explosions, especially the auroras that appeared almost instantaneously far away from the explosion in the opposite hemisphere, were not clearly understood. The nature of the possible radiation belts that were initially generated along the magnetic field lines connecting the areas of the auroral displays were also poorly understood. Areas of blackout of radio communication needed to be understood in much more detail since that information would be critical for military operations during periods of possible nuclear explosions. The Fishbowl tests were monitored by a large number of surface and aircraft-based stations in the wide area around the planned detonations and also in the region in the southern hemisphere in the Samoan Islands region, which was known in these tests as the southern conjugate region. Johnston Island is in the northern hemisphere, as were all of the planned Operation Fishbowl nuclear detonation locations. It was known from previous high altitude tests, as well as from theoretical work done in the late 1950s, that high-altitude nuclear tests produce a number of unique geophysical phenomena at the opposite end of the magnetic field line of the Earth's magnetic field. According to the standard reference book on nuclear weapon effects by the United States Department of Defense, "For the high-altitude tests conducted in 1958 and 1962 in the vicinity of Johnston Island, the charged particles entered the atmosphere in the northern hemisphere between Johnston Island and the main Hawaiian Islands, whereas the conjugate region was in the vicinity of the Samoan, Fiji, and Tonga Islands. It is in these areas that auroras were actually observed, in addition to those in the areas of the nuclear explosions." Beta particles are charged particles (usually with a negative electrical charge) that are released from nuclear explosions. These particles travel in a spiral along the magnetic field lines in the Earth's magnetic field. The nuclear explosions also release heavier debris ions, which also carry an electrical charge, and which also travel in a spiral along the Earth's magnetic field lines. The Earth's magnetic field lines arc high above the Earth until they reach the magnetic conjugate area in the opposite hemisphere. According to the DOD nuclear weapon effects reference, "Because the beta particles have high velocities, the beta auroras in the remote (southern) hemisphere appeared within a fraction of a second of those in the hemisphere where the burst had occurred. The debris ions, however, travel more slowly and so the debris aurora in the remote hemisphere, if it is formed, appears at a somewhat later time. The beta auroras are generally most intense at an altitude of 30 to 60 miles, whereas the intensity of the debris auroras is greatest in the 60 to 125 miles range. Remote conjugate beta auroras can occur if the detonation is above 25 miles, whereas debris auroras appear only if the detonation altitude is in excess of some 200 miles." Some of the charged particles traveling along the Earth's magnetic field lines cause auroras and other geophysical phenomena in the conjugate areas. Other charged particles are reflected back along the magnetic field lines, where they can persist for long periods of time (up to several months or longer), forming artificial radiation belts. According to the Operation Fishbowl planning document of November 1961, "Since much valuable data can be obtained from time and spectrum resolved photography, this dictates that the test be performed at nighttime when auroral photographic conditions are best." As with all U.S. Pacific high-altitude nuclear tests, all of the Operation Fishbowl tests were completed at night. This is in contrast to the high-altitude nuclear tests of the Soviet Project K nuclear tests, which were done over the populated land region of central Kazakhstan, and therefore had to be done during the daytime to avoid eyeburn damage to the population from the very bright flash of high-altitude nuclear explosions (as discussed in the introduction to this article). First attempts According to the initial plan of Operation Fishbowl, the nuclear tests were to be Bluegill, Starfish and Urraca, in that order. If a test were to fail, the next attempt of the same test would be of the same name plus the word "prime." If Bluegill failed, the next attempt would be Bluegill Prime, and if Bluegill Prime failed, the next attempt would be Bluegill Double Prime, etc. Bluegill The first planned test of Operation Fishbowl was on June 2, 1962 when a nuclear warhead was launched from Johnston Island on a Thor missile just after midnight. Although the Thor missile appeared to be on a normal trajectory, the radar tracking system lost track of the missile. Because of the large number of ships and aircraft in the area, there was no way to predict if the missile was on a safe trajectory, so the range safety officers ordered the missile with its warhead to be destroyed. No nuclear detonation occurred and no data was obtained, but subsequent investigation found that the Thor was actually following the proper flight trajectory. Starfish The second planned test of Operation Fishbowl was on June 19, 1962. The launch of a Thor missile with a nuclear warhead occurred just before midnight from Johnston Island. The Thor missile flew a normal trajectory for 59 seconds; then the rocket engine suddenly stopped, and the missile began to break apart. The range safety officer ordered the destruction of the missile and the warhead. The missile was between 30,000 and 35,000 feet (between 9.1 and 10.7 km) in altitude when it was destroyed. Some of the missile parts fell on Johnston Island, and a large amount of missile debris fell into the ocean in the vicinity of the island. Navy Explosive Ordnance Disposal and Underwater Demolition Team swimmers recovered approximately 250 pieces of the missile assembly during the next two weeks. Some of the debris was contaminated with plutonium. Nonessential personnel had been evacuated from Johnston Island during the test. Starfish Prime On July 9, 1962, at 09:00:09 Coordinated Universal Time, which was nine seconds after 10 p.m. on July 8, Johnston Island local time, the Starfish Prime test was successfully detonated at an altitude of . The coordinates of the detonation were 16 degrees, 28 minutes North latitude, 169 degrees, 38 minutes West longitude (30 km, or about 18 mi, southwest of Johnston Island). The actual weapon yield was very close to the design yield, which has been described by various sources at different values in the very narrow range of 1.4 to 1.45 megatons (6.0 PJ). The Thor missile carrying the Starfish Prime warhead actually reached an apogee (maximum height) of about 1100 km (just over 680 miles), and the warhead was detonated on its downward trajectory when it had fallen to the programmed altitude of . The nuclear warhead detonated at 13 minutes and 41 seconds after liftoff of the Thor missile. Starfish Prime caused an electromagnetic pulse (EMP) which was far larger than expected, so much larger that it drove much of the instrumentation off scale, causing great difficulty in getting accurate measurements. The Starfish Prime electromagnetic pulse also made those effects known to the public by causing electrical damage in Hawaii, about away from the detonation point, knocking out about 300 streetlights, setting off numerous burglar alarms and damaging a telephone company microwave link (the detonation time was nine seconds after 11 p.m. in Hawaii). A total of 27 sounding rockets were launched from Johnston Island to obtain experimental data from the shot, with the first of the support rockets being launched 2 hours and 45 minutes before the launch of the Thor missile carrying the nuclear warhead. Most of these smaller instrumentation rockets were launched just after the time of the launch of the main Thor missile carrying the warhead. In addition, a large number of rocket-borne instruments were launched from a firing area at Barking Sands, Kauai, in the Hawaiian Islands. A very large number of United States military ships and aircraft were operating in support of Starfish Prime in the Johnston Island area and across the nearby North Pacific region, including the primary instrumentation ship USAS American Mariner providing measurements conducted by personnel provided by RCA Service Company and Barnes Engineering Company. A few military ships and aircraft were also positioned in the southern conjugate region for the test, which was near the Samoan Islands. In addition, an uninvited observation ship from the Soviet Union was stationed near Johnston Island for the test and another Soviet scientific expeditionary ship was located in the southern conjugate region, permanent features of all future oceanic nuclear testing. After the Starfish Prime detonation, bright auroras were observed in the detonation area as well as in the southern conjugate region on the other side of the equator from the detonation. According to one of the first technical reports, "The visible phenomena due to the burst were widespread and quite intense; a very large area of the Pacific was illuminated by the auroral phenomena, from far south of the south magnetic conjugate area (Tongatapu) through the burst area to far north of the north conjugate area (French Frigate Shoals). ... At twilight after the burst, resonant scattering of light from lithium and other debris was observed at Johnston and French Frigate Shoals for many days confirming the longtime presence of debris in the atmosphere. An interesting side effect was that the Royal New Zealand Air Force was aided in anti-submarine maneuvers by the light from the bomb." The Starfish Prime radiation belt persisted at high altitude for many months and damaged the United States satellites Traac, Transit 4B, Injun I and Telstar I, as well as the United Kingdom satellite Ariel. It also damaged the Soviet satellite Cosmos V. All of these satellites failed completely within several months of the Starfish detonation. There is also evidence that the Starfish Prime radiation belt may have damaged the satellites Explorer 14, Explorer 15 and Relay 1. Telstar I lasted the longest of the satellites that were clearly damaged by the Starfish Prime radiation, with its complete failure occurring on February 21, 1963. In 2010, the United States Defense Threat Reduction Agency issued a report that had been written in support of the United States Commission to Assess the Threat to the United States from Electromagnetic Pulse Attack. The report, entitled "Collateral Damage to Satellites from an EMP Attack," discusses in great detail the satellite damage caused by the Starfish Prime artificial radiation belts as well as other historical nuclear events that caused artificial radiation belts and their effects on many satellites that were then in orbit. The same report also projects the effects of one or more present-day high altitude nuclear explosions upon the formation of artificial radiation belts and the probable resulting effects on satellites that were in orbit as of the year 2010. Bluegill Prime On July 25, 1962, a second attempt was made to launch the Bluegill device, but ended in disaster when the Thor suffered a stuck valve preventing the flow of LOX to the combustion chamber. The engine lost thrust and unburned RP-1 spilled down into the hot thrust chamber, igniting and starting a fire around the base of the missile. With the Thor engulfed in flames, the Range Safety Officer sent the destruct command, which split the rocket and ruptured both fuel tanks, completely destroying the missile and badly damaging the launch pad. The warhead charges also exploded asymmetrically and sprayed the area with the moderately radioactive core materials. Although there was little danger of an accidental nuclear explosion, the destruction of the nuclear warhead on the launch pad caused contamination of the area by alpha-emitting core materials. Burning rocket fuel, flowing through the cable trenches, caused extensive chemical contamination of the trenches and the equipment associated with the cabling in the trenches. The radioactive contamination on Johnston Island was determined to be a major problem, and it was necessary to decontaminate the entire area before the badly damaged launch pad could be rebuilt. Operations pause Operation Fishbowl test operations stopped after the disastrous failure of Bluegill Prime, and most of the personnel not directly involved in the radioactive cleanup and launch pad rebuild on Johnston Island returned to their home stations to await the resumption of tests. According to the Operation Dominic I report, "The enforced pause allowed DOD to replan the remainder of the Fishbowl series. The Urraca event was canceled to avoid further damage to satellites and three new shots were added." A second launch pad was constructed during the operations pause so that Operation Fishbowl could continue in the event of another serious incident. Continuation of the Fishbowl series After a pause of nearly three months, Operation Fishbowl was ready to continue, beginning with another attempt at the Bluegill test. Bluegill Double Prime Eighty-two days after the failure of Bluegill Prime, about 30 minutes before midnight on the night of October 15, 1962, local Johnston Island time (October 16 UTC), another attempt was made at the Bluegill test. The Thor missile malfunctioned and began tumbling out of control about 85 seconds after launch, and the range safety officer ordered the destruction of the missile and its nuclear warhead about 95 seconds after launch. Checkmate On October 19, 1962, at about 90 minutes before midnight (local Johnston Island time), an XM-33 Strypi rocket launched a low-yield nuclear warhead which detonated successfully at an altitude of . It was reported that the yield and burst altitude were very close to those desired, but according to most official documents the exact nuclear yield remains classified. It is reported in the open literature as simply being less than 20 kilotons. One report by the U.S. federal government, however, reported the Checkmate test yield as 10 kilotons. It was reported that, "Observers on Johnston Island saw a green and blue circular region surrounded by a blood-red ring formed overhead that faded in less than one minute. Blue-green streamers and numerous pink striations formed, the latter lasting for 30 minutes. Observers at Samoa saw a white flash, which faded to orange and disappeared in about one minute." Bluegill Triple Prime The fourth attempt at the Bluegill test was launched on a Thor missile on October 25, 1962 (Johnston Island time). It resulted in a successful detonation of a submegaton nuclear warhead at about one minute before midnight, local time (the official Coordinated Universal Time was 0959 on October 26, 1962). It was officially reported as being in the submegaton range (meaning more than 200 kilotons but less than one megaton), and most observers of the U.S. nuclear testing programs believe that the nuclear yield was about 400 kilotons. One report by the U.S. federal government reported the test yield as 200 kilotons. Since all of the Operation Fishbowl tests were planned to occur during the night, the potential for eyeburn, especially for permanent retinal damage, was an important consideration at all levels of planning. Much research went into the potential eyeburn problem. One of the official reports for the project stated that, for the altitudes planned for the Bluegill, Kingfish and Checkmate tests, "the thermal-pulse durations are of the same order of magnitude or shorter than the natural blink period which, for the average person, is about 150 milliseconds. Furthermore, the atmospheric attenuation is normally much less for a given distance than in the case of sea-level or near-sea-level explosions. Consequently, the eye-damage hazard is more severe." Two cases of retinal damage did occur with military personnel on Johnston Island during the Bluegill Triple Prime test. Neither individual had his protective goggles in place at the instant of the detonation. One official report stated, "In the first case, acuity for central vision was 20/400 initially, but returned to 20/25 by six months. The second victim was less fortunate, as central vision did not improve beyond 20/60. The lesion diameters were 0.35 and 0.50 mm respectively. Both individuals noted immediate visual disturbances, but neither was incapacitated." There had been concern that eyeburn problems might occur during the earlier Starfish Prime test, since the countdown was rebroadcast by radio stations in Hawaii, and many civilians would be watching the thermonuclear detonation as it occurred, but no such problems in Hawaii were reported. Kingfish The Kingfish detonation occurred at 0210 (Johnston Island time) on November 1, 1962 and was the fourth successful detonation of the Fishbowl series. It was officially reported only as being a submegaton explosion (meaning in the range of more than 200 kilotons, but less than a megaton), but most independent observers believe that it used the same 400 kiloton warhead as the Bluegill Triple Prime test, although one report by the U.S. federal government reported the test yield as 200 kilotons. As with the other Fishbowl tests, a number of small rockets with various scientific instrumentation were launched from Johnson Island to monitor the effects of the high-altitude explosion. In the case of the Kingfish test, 29 rockets were launched from Johnston Island in addition to the Thor rocket carrying the nuclear warhead. According to the official report, at the time of the Kingfish detonation, "Johnston Island observers saw a yellow-white, luminous circle with intense purple streamers for the first minute. Some of the streamers displayed what appeared to be a rapid twisting motion at times. A large pale-green patch appeared somewhat south of the burst and grew, becoming the dominant visible feature after 5 minutes. By H+1 the green had become dull gray, but the feature persisted for 3 hours. At Oahu a bright flash was observed and after about 10 seconds a great white ball appeared to rise slowly out of the sea and was visible for about 9 minutes." After most of the electromagnetic pulse measurements on Starfish Prime had failed because the EMP was so much larger than expected, extra care was taken to obtain accurate EMP measurements on the Bluegill Triple Prime and Kingfish tests. The EMP mechanism that had been hypothesized before Operation Fishbowl had been conclusively disproven by the Starfish Prime test. Prompt gamma ray output measurements on these later tests were also carefully obtained so that a new theory of the mechanism for high-altitude EMP could be developed and confirmed. That new theory about the generation of nuclear EMP was developed by Los Alamos physicist Conrad Longmire in 1963, and it is the high-altitude nuclear EMP theory that is still used today. As of the beginning of 2011, the EMP waveforms and prompt gamma radiation outputs for Bluegill Triple Prime and Kingfish remain classified. An unclassified report confirms that these measurements were successfully made and that a subsequent theory (which is the one now used) was developed which describes the mechanism by which the high-altitude EMP is generated. That new theory does give results which are consistent with both the Bluegill Triple Prime and Kingfish data. (The report actually using the Bluegill Triple Prime and Kingfish data to confirm the new EMP theory is the still-classified Part 2 of the unclassified report by Conrad Longmire.) According to a Sandia National Laboratories report, EMP generated during the Operation Fishbowl tests caused "... input circuit troubles in radio receivers during the Starfish and Checkmate bursts; the triggering of surge arresters on an airplane with a trailing-wire antenna during Starfish, Checkmate, and Bluegill; and the Oahu streetlight incident." (The "Oahu streetlight incident" refers to the 300 streetlights in Honolulu extinguished by the Starfish Prime detonation.) Tightrope The final test of Operation Fishbowl was detonated at 2130 (9:30 p.m. local Johnston Island time) on November 3, 1962 (the time and date was officially recorded as 0730 UTC, November 4, 1962). It was launched on a Nike-Hercules missile, and detonated at a lower altitude than the other Fishbowl tests. Although it was officially one of the Operation Fishbowl tests, it is sometimes not listed among high-altitude nuclear tests because of its lower detonation altitude. The nuclear yield was reported in most official documents only as being less than 20 kilotons. One report by the U.S. federal government reported the Tightrope test yield as 10 kilotons. "At Johnston Island, there was an intense white flash. Even with high-density goggles, the burst was too bright to view, even for a few seconds. A distinct thermal pulse was also felt on the bare skin. A yellow-orange disc was formed, which transformed itself into a purple doughnut. A glowing purple cloud was faintly visible for a few minutes." Seven rockets carrying scientific instrumentation were launched from Johnston Island in support of the Tightrope test, which was the final atmospheric test conducted by the United States. Table See also Electromagnetism Geomagnetic storm References External links Joint Task Force 8 video report on Operation Fishbowl Explosions in 1962 1962 in military history 1962 in the United States Johnston Atoll American nuclear explosive tests Exoatmospheric nuclear weapons testing Electromagnetic radiation Energy weapons Bombs Electronic warfare

3037081

https://en.wikipedia.org/wiki/901%20Brunsia

901 Brunsia

901 Brunsia is an S-type asteroid belonging to the Flora family in the Main Belt. Its rotation period is 3.136 hours. References External links 000901 Discoveries by Max Wolf Named minor planets 000901 19180830

3037083

https://en.wikipedia.org/wiki/902%20Probitas

902 Probitas

902 Probitas is a minor planet orbiting the Sun. It was discovered by an Austrian astronomer Johann Palisa in Vienna on 3 September 1918. References External links 000902 Discoveries by Johann Palisa Named minor planets 19180903

3037084

https://en.wikipedia.org/wiki/903%20Nealley

903 Nealley

903 Nealley is a minor planet orbiting the Sun. The semi-major axis of the orbit of 903 Nealley lies just inside the Hecuba gap, located at 3.27 AU. References External links Lightcurve plot of 903 Nealley, Palmer Divide Observatory, B. D. Warner (2011) Asteroid Lightcurve Database (LCDB), query form (info ) Dictionary of Minor Planet Names, Google books Asteroids and comets rotation curves, CdR – Observatoire de Genève, Raoul Behrend Discovery Circumstances: Numbered Minor Planets (1)-(5000) – Minor Planet Center 000903 Discoveries by Johann Palisa Named minor planets 19180913

3037086

https://en.wikipedia.org/wiki/904%20Rockefellia

904 Rockefellia

904 Rockefellia (prov. designation: or ) is a dark and large background asteroid from the outer regions of the asteroid belt, that measures approximately in diameter. It was discovered on 29 October 1918, by German astronomer Max Wolf at the Heidelberg-Königstuhl State Observatory. The carbonaceous C-type asteroid (Ch) has a rotation period of 6.8 hours and is rather spherical in shape. It was named after American philanthropist and oil industrialist John D. Rockefeller (1839–1937). Orbit and classification Rockefellia is a non-family asteroid of the main belt's background population when applying the hierarchical clustering method to its proper orbital elements. It orbits the Sun in the outer asteroid belt at a distance of 2.7–3.3 AU once every 5 years and 2 months (1,895 days; semi-major axis of 3 AU). Its orbit has an eccentricity of 0.09 and an inclination of 15° with respect to the ecliptic. The asteroid was first observed as () at the Simeiz Observatory on 28 October 1913, and three nights later at Heidelberg Observatory as well. The body's observation arc begins at Heidelberg on 6 December 1918, or five weeks after its official discovery observation. Naming This minor planet was named after John D. Rockefeller (1839–1937), an American philanthropist and oilman who founded the Rockefeller Foundation. The official was mentioned in The Names of the Minor Planets by Paul Herget in 1955 (). Physical characteristics In the Tholen- and SMASS-like taxonomy of the Small Solar System Objects Spectroscopic Survey (S3OS2), Rockefellia is a Caa and Ch type, respectively, both indicating that it is a hydrated, carbonaceous C-type asteroid. Rotation period In December 2017, a rotational lightcurve of Rockefellia was obtained from photometric observations by Tom Polakis at the Command Module Observatory in Arizona. Lightcurve analysis gave a rotation period of hours with a low brightness variation of magnitude (). The result supersedes tentative period determinations by Pierre Antonini (2009), Stephane Fauvaud (2011) and René Roy (2014), which were of lower quality (). Diameter and albedo According to the survey carried out by the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer (WISE), the Infrared Astronomical Satellite IRAS, and the Japanese Akari satellite, Rockefellia measures (), () and () kilometers in diameter and its surface has an albedo of (), () and (), respectively. The Collaborative Asteroid Lightcurve Link derives an albedo of 0.0357 and calculates a diameter of 58.51 kilometers based on an absolute magnitude of 10.4. Alternative mean-diameter measurements published by the WISE team include (), (), () and () with corresponding albedos of (), () and () and (). On 13 May 2005, an asteroid occultation gave a best-fit ellipse dimension of 59.0 × 59.0 kilometers. These timed observations are taken when the asteroid passes in front of a distant star. However the quality of the measurement is rated poorly. A second, lower rated observation on 23 February 2013, measured an ellipse of 61.0 × 61.0 kilometers. References External links Lightcurve Database Query (LCDB), at www.minorplanet.info Dictionary of Minor Planet Names, Google books Asteroids and comets rotation curves, CdR – Geneva Observatory, Raoul Behrend Discovery Circumstances: Numbered Minor Planets (1)-(5000) – Minor Planet Center 000904 Discoveries by Max Wolf Named minor planets 19181029

3037088

https://en.wikipedia.org/wiki/905%20Universitas

905 Universitas

905 Universitas is an S-type asteroid orbiting in the Main belt as part of the Flora family. Its diameter is about 21 km and it has an albedo of 0.085. Its rotation period is approximately 14.2 hours. References External links 000905 Discoveries by Friedrich Karl Arnold Schwassmann Named minor planets 000905 19181030

3037090

https://en.wikipedia.org/wiki/906%20Repsolda

906 Repsolda

906 Repsolda is a minor planet orbiting the Sun. It is named for the German astronomer and fireman Johann Georg Repsold (1770–1830), who founded and ran Hamburg Observatory. References External links 000906 Discoveries by Friedrich Karl Arnold Schwassmann Named minor planets 19181030

3037098

https://en.wikipedia.org/wiki/907%20Rhoda

907 Rhoda

907 Rhoda is a large background asteroid from the central region of the asteroid belt, that measures approximately in diameter. It was discovered on 12 November 1918, by astronomer Max Wolf at the Heidelberg Observatory in southwest Germany. The dark C/X-type asteroid has a long rotation period of 22.4 hours and is likely spherical in shape. It was named after Rhoda Barnard, wife of American astronomer Edward Emerson Barnard (1857–1923). Orbit and classification Rhoda is a non-family asteroid of the main belt's background population when applying the hierarchical clustering method to its proper orbital elements. It orbits the Sun in the central asteroid belt at a distance of 2.3–3.3 AU once every 4 years and 8 months (1,712 days; semi-major axis of 2.8 AU). Its orbit has an eccentricity of 0.16 and an inclination of 20° with respect to the ecliptic. The body's observation arc begins with its first observation as () at the Heidelberg-Königstuhl State Observatory on 18 January 1901, where it was officially discovered almost 18 years later on 12 November 1918. Naming This minor planet was named after Rhoda Barnard (née Calvert), wife of the American astronomer Edward Emerson Barnard (1857–1923), who was himself honored with the asteroid 819 Barnardiana. The official naming was published in the journal Astronomische Nachrichten in 1922 (AN 215, 471). The was also mentioned in The Names of the Minor Planets by Paul Herget in 1955 (). Physical characteristics In the Tholen classification, Rhoda is a common, carbonaceous C-type asteroid, while in the Bus–Binzel SMASS classification it is a Xk-subtype, which transitions from the X-type to the uncommon K-type asteroids. In the Barucci-taxonomy, which classified a total of 438 asteroids in 1987, Rhoda is a C0-type. Rotation period In April 2004, a rotational lightcurve of Rhoda was obtained from photometric observations by Brian Warner at the Palmer Divide Observatory in Colorado. Lightcurve analysis gave a rotation period of hours with a low brightness variation of magnitude, indicative of a non-elongated, spherical shape (). Other period determinations were made by Marciniak as well as by Raphaël Nicollerat and Raoul Behrend, giving a low-amplitude lightcurve with a period of and hours, respectively (). Diameter and albedo According to the survey carried out by the Infrared Astronomical Satellite IRAS, the Japanese Akari satellite, and the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer (WISE), Rhoda measures (), () and () kilometers in diameter and its surface has an albedo of (), () and (), respectively. The Collaborative Asteroid Lightcurve Link adopts the results obtained by IRAS, that is, an albedo of 0.0560 and calculates a diameter of 62.73 kilometers based on an absolute magnitude of 10.74. Alternative mean-diameter measurements published by the WISE team include in ascending order (), (), () and () and albedos of (), (), () and (). An asteroid occultation, observed on 23 March 2009, gave a best-fit ellipse dimension of 63.0 × 63.0 kilometers. These timed observations are taken when the asteroid passes in front of a distant star. Notes References External links Lightcurve Database Query (LCDB), at www.minorplanet.info Dictionary of Minor Planet Names, Google books Asteroids and comets rotation curves, CdR – Geneva Observatory, Raoul Behrend Discovery Circumstances: Numbered Minor Planets (1)-(5000) – Minor Planet Center 000907 Discoveries by Max Wolf Named minor planets 000907 000907 19181112

3037102

https://en.wikipedia.org/wiki/908%20Buda

908 Buda

908 Buda (prov. designation: or ) is a background asteroid from the inner regions of the asteroid belt, approximately in diameter. It was discovered by German astronomer Max Wolf at the Heidelberg Observatory on 30 November 1918. The uncommon L-type asteroid has a rotation period of 14.6 hours. It was named after Buda, the smaller part of the Hungarian city of Budapest. Orbit and classification Buda is a non-family asteroid of the main belt's background population when applying the hierarchical clustering method to its proper orbital elements. It orbits the Sun in the inner asteroid belt at a distance of 2.1–2.8 AU once every 3 years and 11 months (1,421 days; semi-major axis of 2.47 AU). Its orbit has an eccentricity of 0.15 and an inclination of 13° with respect to the ecliptic. The body's observation arc begins at Heidelberg Observatory with its official discovery observation on 30 November 1918. Naming This minor planet was named after Buda, the smaller part of the Hungarian capital city of Budapest (the larger part being Pest). It is located on the west bank of the Danube River. The asteroid's citation was mentioned in The Names of the Minor Planets by Paul Herget in 1955 (). Physical characteristics In the Bus–Binzel SMASS classification, Buda is an uncommon L-type, while in the Bus–DeMeo taxonomy, it is a D-type asteroid. Rotation period and poles In March 2009, a rotational lightcurve of Buda was obtained from photometric observations by Brian Warner at his Palmer Divide Observatory in Colorado. Analysis gave a classically shaped bimodal lightcurve with a rotation period of hours and a brightness variation of magnitude (). This supersedes a period determination by French amateur astronomer Laurent Bernasconi from January 2005, who determined a period of hours with an amplitude of magnitude (). Observations by Julian Oey in 2015 gave two similar periods (). In 2016, a modeled lightcurve using photometric data from various sources of an international collaboration of astronomers, rendered a concurring sidereal period of and two spin axes of (40.0°, 5.0°) and (225.0°, 16.0°) in ecliptic coordinates (λ, β). Diameter and albedo According to the survey carried out by the Infrared Astronomical Satellite IRAS, the Japanese Akari satellite, and the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer (WISE), Buda measures (), () and () kilometers in diameter and its surface has an albedo of (), () and (), respectively. The Collaborative Asteroid Lightcurve Link derives an albedo of 0.1509 and calculates a diameter of 24.33 kilometers based on an absolute magnitude of 10.74. Alternative mean-diameter measurements published by the WISE team include () and () with corresponding albedos of () and (). Notes References External links Lightcurve Database Query (LCDB), at www.minorplanet.info Dictionary of Minor Planet Names, Google books Asteroids and comets rotation curves, CdR – Geneva Observatory, Raoul Behrend Discovery Circumstances: Numbered Minor Planets (1)-(5000) – Minor Planet Center 000908 Discoveries by Max Wolf Named minor planets 000908 19181130

3037104

https://en.wikipedia.org/wiki/909%20Ulla

909 Ulla

909 Ulla is a large and dark asteroid from the outermost regions of the asteroid belt, that measures approximately in diameter. It is the parent body and namesake of the Ulla family, which belongs to the larger group of Cybele asteroids. It was discovered on 7 February 1919, by German astronomer Karl Reinmuth at the Heidelberg Observatory in southwest Germany. The X-type asteroid has a rotation period of 8.7 hours and a notably low value for its Jupiter Tisserand's parameter. It was named after Ulla Ahrens, daughter of a friend of the discoverer. Orbit and classification Ulla is the parent body of the Ulla family (), a very small asteroid family of less than 30 known bodies. It orbits the Sun in the outermost asteroid belt at a distance of 3.2–3.9 AU once every 6 years and 8 months (2,435 days; semi-major axis of 3.54 AU). Its orbit has an eccentricity of 0.09 and an inclination of 19° with respect to the ecliptic. Naming This minor planet was named after Ulla Ahrens, a daughter of a friend of the discoverer. Karl Reinmuth also named the asteroid 950 Ahrensa for the Ahrens family, who was a donor of the Heidelberg Observatory. The official naming citation was mentioned in The Names of the Minor Planets by Paul Herget in 1955 (). Physical characteristics In the SMASS classification, Ulla is an X-type asteroid. Rotation period A rotational lightcurve of Ulla was obtained from photometric observations in 2000. Lightcurve analysis gave a rotation period of 8.73 hours with a brightness amplitude between 0.13 and 0.24 magnitude (). Other photometric period determinations gave concurring results. Diameter and albedo According to the surveys carried out by the Infrared Astronomical Satellite IRAS and the Japanese Akari satellite, Ulla measures and kilometers in diameter and its surface has an albedo between and . The Collaborative Asteroid Lightcurve Link uses an albedo of 0.0450 and derives a diameter of 116.66 kilometers based on an absolute magnitude of 8.65. References External links Lightcurve Database Query (LCDB), at www.minorplanet.info Dictionary of Minor Planet Names, Google books Asteroids and comets rotation curves, CdR – Geneva Observatory, Raoul Behrend Discovery Circumstances: Numbered Minor Planets (1)-(5000) – Minor Planet Center 000909 000909 Discoveries by Karl Wilhelm Reinmuth Named minor planets 000909 19190207

3037106

https://en.wikipedia.org/wiki/910%20Anneliese

910 Anneliese

910 Anneliese (prov. designation: or ) is a dark background asteroid, approximately in diameter, located in the outer regions of the asteroid belt. It was discovered on 1 March 1919, by astronomer Karl Reinmuth at the Heidelberg-Königstuhl State Observatory in southwest Germany. The carbonaceous C-type asteroid (Ch) has a rotation period of 11.3 hours and is likely spherical in shape. It was named by German astronomer Julius Dick after his friend "Anneliese". Orbit and classification Anneliese is a non-family asteroid of the main belt's background population when applying the hierarchical clustering method to its proper orbital elements. It orbits the Sun in the outer asteroid belt at a distance of 2.5–3.4 AU once every 5.00 years (1,828 days; semi-major axis of 2.93 AU). Its orbit has an eccentricity of 0.15 and an inclination of 9° with respect to the ecliptic. The body's observation arc begins at Heidelberg Observatory on 19 March 1919, or 18 days after its official discovery observation. Naming This minor planet was named after "Anneliese", an acquaintance of the German astronomer Julius Dick from the Babelsberg Observatory, who suggested the asteroid's name. The was also mentioned in The Names of the Minor Planets by Paul Herget in 1955 (). Physical characteristics In the Bus–Binzel SMASS classification, Anneliese is a hydrated carbonaceous C-type asteroid (Ch). Rotation period In June 2015, a rotational lightcurve of Anneliese was obtained from photometric observations by Uruguayan astronomer Eduardo Álvarez at the Los Algarrobos Observatory . Lightcurve analysis gave a well-defined rotation period of hours with a brightness variation of magnitude, indicative of a spherical, non-elongated shape (). At the time Anneliese was one of only 17 three-digit numbered asteroids for which no period was published. In May 2015, Julian Oey at the Blue Mountains Observatory , Australia, determined a concurring period of hours with an amplitude of magnitude (). In May 2015 a collaboration of Spanish amateur astronomers including Alfonso Garceràn , Amadeo Macias , Enrique Mansego , Pedro Rodriguez and Juan de Haro measured a period of hours—or half the period solution of the other observations, with an amplitude of magnitude (). Diameter and albedo According to the survey carried out by the Infrared Astronomical Satellite IRAS, the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer (WISE), and the Japanese Akari satellite, Anneliese measures (), () and () kilometers in diameter and its surface has an albedo of (), () and (), respectively. The Collaborative Asteroid Lightcurve Link derives an albedo of 0.0505 and a diameter of 46.98 kilometers based on an absolute magnitude of 10.5, while Alvares gives a diameter of () and an albedo of (). An asteroid occultation, observed on 14 September 2012, gave a best-fit ellipse dimension of 48.0 × 48.0 kilometers. These timed observations are taken when the asteroid passes in front of a distant star. However the quality of the measurement is rated poorly. Further published mean-diameters by the WISE team include (), () and () with corresponding albedos of (), () and (). References External links Lightcurve Database Query (LCDB), at www.minorplanet.info Dictionary of Minor Planet Names, Google books Discovery Circumstances: Numbered Minor Planets (1)-(5000) – Minor Planet Center 000910 Discoveries by Karl Wilhelm Reinmuth Named minor planets 000910 19190301

3037110

https://en.wikipedia.org/wiki/911%20Agamemnon

911 Agamemnon

911 Agamemnon, provisional designation , is a large Jupiter trojan and a suspected binary asteroid from the Greek camp, approximately in diameter. It was discovered on 19 March 1919, by German astronomer Karl Reinmuth at the Heidelberg Observatory in southwest Germany. The dark D-type asteroid is one of the largest Jupiter trojans and has a rotation period of 6.6 hours. It is named after the Greek King Agamemnon, a main character of the Iliad. Orbit and classification Agamemnon is a dark Jovian asteroid orbiting in the Greek camp at Jupiter's leading Lagrangian point, 60° ahead of its orbit in a 1:1 resonance . It is also a non-family asteroid in the Jovian background population. It orbits the Sun at a distance of 4.9–5.6 AU once every 12 years and 1 month (4,427 days; semi-major axis of 5.28 AU). Its orbit has an eccentricity of 0.07 and an inclination of 22° with respect to the ecliptic. The body's observation arc begins at Heidelberg in October 1927, more than 8 years after its official discovery observation. Physical characteristics In the Tholen classification, Agamemnon is a dark D-type asteroid. It has also been characterized as a D-type in both the Tholen- and SMASS-like taxonomy of the Small Solar System Objects Spectroscopic Survey (S3OS2). Rotation period Photometric observations of this asteroid during 1997 were used to build a lightcurve showing a rotation period of hours with a brightness variation of magnitude. A 2009 study yielded a period of hours, in reasonable agreement with the previous result. Diameter and albedo According to the surveys carried out by the Infrared Astronomical Satellite IRAS, the Japanese Akari satellite and the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer, Agamemnon measures between 131.04 and 185.30 kilometers in diameter, based on a common absolute magnitude of 7.89 and a surface albedo between 0.037 and 0.072. A concurring diameter estimate of kilometers from an occultation event (see below) has also been obtained. The Collaborative Asteroid Lightcurve Link agrees with the results obtained by IRAS, that is, an albedo of 0.0444 and a diameter of 166.66 kilometers based on an absolute magnitude of 7.89. Shape and satellite A 2012 occultation produced a 2D shape model of roughly (with an irregular, skewed outline) and are suggestive of Agamemnon to have a satellite of approximately kilometers in diameter orbiting at from the primary's center. Naming This minor planet named from Greek mythology after King Agamemnon, the leader of the Greeks in the Trojan War. He is a main character of Homer's Iliad. The official naming citation was mentioned in The Names of the Minor Planets by Paul Herget in 1955 (). Notes References External links Asteroid Lightcurve Database (LCDB), query form (info ) Dictionary of Minor Planet Names, Google books Discovery Circumstances: Numbered Minor Planets (1)-(5000) – Minor Planet Center 000911 Discoveries by Karl Wilhelm Reinmuth Named minor planets 000911 19190319 Agamemnon

3037111

https://en.wikipedia.org/wiki/912%20Maritima

912 Maritima

912 Maritima is an asteroid in the asteroid belt. Based on lightcurve studies observing Maritima over a three-month period, Maritima has a rotation period of 1332 hours. Analysis reveals a possible synodic period of . Superslow rotators, those with periods longer than a few days, are generally small asteroids. The current paradigm is that slowing of an asteroid's spin rate is the result of YORP radiation pressure, which acts on the target as the inverse square of its size and the inverse of its semi-major axis. The rotation period is less than conclusive. References External links Lightcurve plot of 912 Maritima, Palmer Divide Observatory, B. D. Warner (2005) Asteroid Lightcurve Database (LCDB), query form (info ) Dictionary of Minor Planet Names, Google books Asteroids and comets rotation curves, CdR – Observatoire de Genève, Raoul Behrend Discovery Circumstances: Numbered Minor Planets (1)-(5000) – Minor Planet Center 000912 Discoveries by Friedrich Karl Arnold Schwassmann Named minor planets 000912 000912 19190427

3037113

https://en.wikipedia.org/wiki/913%20Otila

913 Otila

913 Otila (prov. designation: or ) is a bright Flora asteroid from the inner regions of the asteroid belt. It was discovered by German astronomer Karl Reinmuth at the Heidelberg Observatory on 19 May 1919. The stony S-type asteroid has a short rotation period of 4.9 hours and measures approximately in diameter. It was named after a common German female name unrelated to the discoverer's contemporaries, that was taken from the almanac Lahrer Hinkender Bote. Orbit and classification When applying the synthetic hierarchical clustering method (HCM) by Nesvorný, or the 1995 HCM-analysis by Zappalà, Otila is a member of the Flora family (), a giant asteroid family and the largest family of stony asteroids in the main-belt. However, according to another HCM-analysis by Milani and Knežević (AstDys), it is a background asteroid as this analysis does not recognize the Flora asteroid clan. Otila orbits the Sun in the inner main-belt at a distance of 1.8–2.6 AU once every 3 years and 3 months (1,190 days; semi-major axis of 2.2 AU). Its orbit has an eccentricity of 0.17 and an inclination of 6° with respect to the ecliptic. The body's observation arc begins with its first observation as () at Heidelberg Observatory in April 1909, more than 10 year prior to its official discovery observation. Naming This minor planet was named "Otila", after a female name picked from the Lahrer Hinkender Bote, published in Lahr, southern Germany. A Hinkender Bote (lit. "limping messenger") was a very popular almanac, especially in the alemannic-speaking region from the late 17th throughout the early 20th century. The calendar section contains feast days, the dates of important fairs and astronomical ephemerides. For 26 February, the calendar gives "Otila" as the German name day analogue next to Hestor and Alexander, the protestant and catholic entries in the calendar of saints, latter likely referring to Pope Alexander I of Alexandria, whose feast day is also 26 February. Reinmuth's calendar names Otila is the first in a series of 23 asteroids – ending with 1144 Oda – for which Reinmuth used the Lahrer Hinkender Bote to select names from, as he had trouble thinking of proper names due to his many asteroid discoveries. These names are not related to the discoverer's contemporaries. Lutz Schmadel, the author of the Dictionary of Minor Planet Names learned about Reinmuth's source of inspiration from private communications with Dutch astronomer Ingrid van Houten-Groeneveld, who worked as a young astronomer at Heidelberg. Physical characteristics In the Bus–Binzel SMASS classification, Otila is an Sa-subtype that transitions from a common, stony S-type to an uncommon A-type asteroid, while in the Bus-DeMeo-taxonomy, it is an Sw-type asteroid, where the "w" notation is used for a objects with a high spectral slope (greater than 0.25). Rotation period In April 2007, a rotational lightcurve of Otila was obtained from photometric observations by Julian Oey. Lightcurve analysis gave a rotation period of hours with a brightness amplitude of magnitude (). Diameter and albedo According to the survey carried out by the Japanese Akari satellite and the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer (WISE), Otila measures () and () kilometers in diameter and its surface has an albedo of () and (), respectively. The Collaborative Asteroid Lightcurve Link assumes a standard albedo for members of the Flora family of 0.24 and calculates a diameter of 10.80 kilometers based on an absolute magnitude of 12.0. Other publications by the WISE team give a mean-diameter of () and () kilometers with a corresponding albedo of () and (). References External links Do Slivan states exist in the Flora family?. I. Photometric survey of the Flora region, Astronomy & Astrophysics, A. Kryszczynska Lightcurve Database Query (LCDB), at www.minorplanet.info Dictionary of Minor Planet Names, Google books Discovery Circumstances: Numbered Minor Planets (1)-(5000) – Minor Planet Center 000913 Discoveries by Karl Wilhelm Reinmuth Named minor planets 000913 19190519

3037114

https://en.wikipedia.org/wiki/914%20Palisana

914 Palisana

914 Palisana, provisional designation , is a Phocaean asteroid from the inner regions of the asteroid belt, approximately 77 kilometers in diameter. It was discovered by German astronomer Max Wolf at Heidelberg Observatory on 4 July 1919. Description The carbonaceous asteroid is classified as a CU-type on the Tholen taxonomic scheme. It orbits the Sun at a distance of 1.9–3.0 AU once every 3 years and 10 months (1,407 days). Its orbit has an eccentricity of 0.21 and an inclination of 25° with respect to the ecliptic. Measurements using the adaptive optics at the W. M. Keck Observatory give a diameter estimate of 76 km. The size ratio between the major and minor axes is 1.16. During 2004, the asteroid was observed occulting a star. The resulting chords were used to determine a diameter estimate of 91.2 km. This is a poor match to the diameter determined by other means. The minor planet is named after the Austrian astronomer Johann Palisa (1848–1925), who has discovered many asteroids himself between 1874 and 1923. References External links Lightcurve plot of 914 Palisana, Palmer Divide Observatory, B. D. Warner (2008) Asteroid Lightcurve Database (LCDB), query form (info ) Dictionary of Minor Planet Names, Google books Asteroids and comets rotation curves, CdR – Observatoire de Genève, Raoul Behrend Discovery Circumstances: Numbered Minor Planets (1)-(5000) – Minor Planet Center 000914 Discoveries by Max Wolf Named minor planets 000914 19190704

3037116

https://en.wikipedia.org/wiki/915%20Cosette

915 Cosette

915 Cosette is an S-type asteroid belonging to the Flora family of Main Belt asteroids. Its rotation period is 4.445 hours. References External links 000915 000915 Discoveries by François Gonnessiat Named minor planets 000915 19181214

3037118

https://en.wikipedia.org/wiki/916%20America

916 America

916 America is a minor planet orbiting the Sun in the main belt between Mars and Jupiter. It was discovered on 7 August 1915 by the Russian astronomer Grigory Nikolaevich Neujmin at Simeis, Russian Empire. Originally designated 916ΣI, it was renamed '916 America' on 24 February 1923 after the Council of Astronomers at Pulkovo Observatory decided to commemorate "the friendly relations of the astronomical observatories and astronomers". Another possible reason for the name was as a mark of appreciation for the help given during the 1921 Russian famine by the American Relief Administration under the later President Herbert Hoover. In 1986, assuming that the asteroid was of S-type and that it had a diameter of 15 km, the rotational period was measured to be 38 hours. Observations by the Infrared Astronomical Satellite have since shown that it has a diameter of 33.2±1.3 km, with an absolute magnitude of 11.20 and an albedo of 0.053±0.004. References External links 000916 Discoveries by Grigory Neujmin Named minor planets 19150807

3037120

https://en.wikipedia.org/wiki/917%20Lyka

917 Lyka

917 Lyka (prov. designation: or ) is a background asteroid, approximately in diameter, located in the inner region of the asteroid belt. It was discovered on 5 September 1915, by Russian astronomer Grigory Neujmin at the Simeiz Observatory on the Crimean peninsula. The X-type asteroid has a rotation period of 7.9 hours and is likely spherical in shape. It was named after Lyka, a friend of the discoverer's sister. Orbit and classification Lyka is a non-family asteroid of the main belt's background population when applying the hierarchical clustering method to its proper orbital elements. It orbits the Sun in the inner main-belt at a distance of 1.9–2.9 AU once every 3 years and 8 months (1,342 days; semi-major axis of 2.38 AU). Its orbit has an eccentricity of 0.20 and an inclination of 5° with respect to the ecliptic. The body's observation arc begins at Simeiz on 1 September 1926, eleven years after to its official discovery observation. Naming This minor planet was named after Lyka, a friend of the sister of discoverer Grigory Neujmin. Lutz Schmadel, the author of the Dictionary of Minor Planet Names learned about the meaning of the asteroid's name from private communications with long-time Simeiz astronomer Nikolai Chernykh. Physical characteristics In both the Tholen- and SMASS-like taxonomy of the Small Solar System Objects Spectroscopic Survey (S3OS2), Lyka is an X-type asteroid. Rotation period In January 2005, a rotational lightcurve of Lyka was obtained from photometric observations by Matthieu Conjat. Lightcurve analysis gave a well-defined rotation period of hours with a low brightness variation of magnitude, indicative of a rather spherical shape (). In October 2018, the period was confirmed by Laurent Bernasconi () and by Alfonso Carreño of OBAS () with amplitudes of and , respectively (). Diameter and albedo According to the survey carried out by the Infrared Astronomical Satellite IRAS, the Japanese Akari satellite, and the NEOWISE mission of NASA's WISE telescope (WISE), Lyka measures (), () and () kilometers in diameter and its surface has an albedo of (), () and (), respectively. The Collaborative Asteroid Lightcurve Link derives an albedo of 0.0520 and a diameter of 27.89 km based on an absolute magnitude of 11.6. Further published mean-diameters by the WISE team include (), (), () and () with albedos between () and (). An asteroid occultation, observed on 4 March 2005, gave a best-fit ellipse dimension of 28.0×28.0 kilometers. These timed observations are taken when the asteroid passes in front of a distant star. However the quality of the measurement is rated poorly. References External links Lightcurve Database Query (LCDB), at www.minorplanet.info Dictionary of Minor Planet Names, Google books Asteroids and comets rotation curves, CdR – Geneva Observatory, Raoul Behrend Discovery Circumstances: Numbered Minor Planets (1)-(5000) – Minor Planet Center 000917 Discoveries by Grigory Neujmin Named minor planets 19150905

3037121

https://en.wikipedia.org/wiki/918%20Itha

918 Itha

918 Itha (prov. designation: or ) is a stony asteroid and the namesake as well as the principal body of the Itha family, located in the outer region of the asteroid belt. It was discovered by German astronomer Karl Reinmuth at the Heidelberg Observatory on 22 August 1919. The S-type asteroid has a notably short rotation period of only 3.5 hours and measures approximately in diameter. It was named "Itha", a female name taken from the almanac Lahrer Hinkender Bote, unrelated to the discoverer's contemporaries. Orbit and classification When applying the synthetic hierarchical clustering method (HCM) by Nesvorný, Itha is the principal body and namesake of the Itha family (), a small family of stony asteroids with only a few dozen known members. Other larger and low-numbered members of this family include 968 Petunia, 1067 Lunaria, 3787 Aivazovskij, 4119 Miles and 5232 Jordaens. However, according to another HCM-analysis by Milani and Knežević (AstDys), Itha is a background asteroid as it is not a legitimate family in their analysis. It orbits the Sun in the outer asteroid belt at a distance of 2.3–3.4 AU once every 4 years and 10 months (1,770 days; semi-major axis of 2.86 AU). Its orbit has an eccentricity of 0.19 and an inclination of 12° with respect to the ecliptic. Itha was first observed as () at the U.S. Taunton Observatory in Massachusetts. The body's observation arc begins at Heidelberg Observatory on 23 August 1919, the night after its official discovery observation. Naming This minor planet was named "Itha", picked from the Lahrer Hinkender Bote, an almanac which was published in Lahr, southern Germany. Especially in the alemannic-speaking region, a Hinkender Bote (lit. "limping messenger") was very popular from the late 17th throughout the early 20th century. The calendar section contains feast days, the dates of important fairs and astronomical ephemerides. For 15 January, the calendar gives "Itha" as the German name day analogue next to Maurus and Habakuk, the protestant and catholic entries in the calendar of saints, likely referring to Saint Maurus and prophet Habakkuk. Reinmuth's calendar names As with 22 other asteroids – starting with 913 Otila, and ending with 1144 Oda – Reinmuth selected names from this calendar due to his many asteroid discoveries that he had trouble thinking of proper names. These names are not related to the discoverer's contemporaries. Lutz Schmadel, the author of the Dictionary of Minor Planet Names learned about Reinmuth's source of inspiration from private communications with Dutch astronomer Ingrid van Houten-Groeneveld, who worked as a young astronomer at Heidelberg. Physical characteristics Itha is an S-type asteroid in the SMASS-I classification by Xu (1995). This agrees with the overall spectral type for members of the Itha family. Rotation period In June 2011, a rotational lightcurve of Itha was obtained from photometric observations by Julian Oey at Kingsgrove Observatory , Australia, in collaboration with three Argentinian astronomers. Lightcurve analysis gave a well-defined rotation period of hours with a brightness variation of magnitude (). Two modeled lightcurves using photometric data from the Lowell Photometric Database and from the BlueEye600 robotic telescope at Ondřejov Observatory gave a sidereal period of and , respectively. The modelling of the former gave two poles at (59.0°, −59.0°) and (249.0°, −72.0°), while the one of the latter gave only one pole at (72.0°, −54.0°) in ecliptic coordinates (λ, β). Diameter and albedo According to the surveys carried out by the Infrared Astronomical Satellite IRAS, the Japanese Akari satellite, and the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer (WISE), Itha measures (), () and () kilometers in diameter, and its surface has an albedo of (), () and (), respectively. The Collaborative Asteroid Lightcurve Link derives an albedo of 0.2412 and a diameter of 20.53 km based on an absolute magnitude of 10.6. Other published mean-diameters by the WISE team include () and () with corresponding albedos of () and (). References External links Lightcurve Database Query (LCDB), at www.minorplanet.info Dictionary of Minor Planet Names, Google books Discovery Circumstances: Numbered Minor Planets (1)-(5000) – Minor Planet Center 000918 Discoveries by Karl Wilhelm Reinmuth Named minor planets 19190822

3037124

https://en.wikipedia.org/wiki/919%20Ilsebill

919 Ilsebill

919 Ilsebill (prov. designation: or ) is a dark background asteroid from the central region of the asteroid belt. It was discovered on 30 October 1918, by astronomer Max Wolf at the Heidelberg-Königstuhl State Observatory in southwest Germany. The carbonaceous C-type asteroid has a short rotation period of 5.0 hours and measures approximately in diameter. It was named after "Ilsebill", a character in the fairy tale The Fisherman and his Wife by the Brothers Grimm. Orbit and classification Ilsebill is a non-family asteroid of the main belt's background population when applying the hierarchical clustering method to its proper orbital elements. It orbits the Sun in the central asteroid belt at a distance of 2.5–3.0 AU once every 4 years and 7 months (1,686 days; semi-major axis of 2.77 AU). Its orbit has an eccentricity of 0.08 and an inclination of 8° with respect to the ecliptic. The body's observation arc begins at Heidelberg Observatory with its official discovery observation on 30 October 1918. Naming This minor planet was named after the character "Ilsebill" in the fairy tale The Fisherman and his Wife () by the Brothers Grimm. The asteroid was named likely after the discoverer's death in 1932, upon a proposal made by his widow , and subsequently published by ARI (). The was also mentioned in The Names of the Minor Planets by Paul Herget in 1955 (). Physical characteristics In the Bus–Binzel SMASS classification and in the SDSS-based taxonomy, Ilsebill is a common, carbonaceous C-type asteroid. Rotation period In October 2010, a rotational lightcurve of Ilsebill was obtained from photometric observations by Zachary Pligge, Ben Hall and Richard Ditteon at the U.S. Oakley Observatory in Indiana. Lightcurve analysis gave a well-defined rotation period of hours with a brightness variation of magnitude (). In September 2010, a similar, though lower rated period of hours with an amplitude of was determined by astronomers at the Palomar Transient Factory in California (). A modeled lightcurve using photometric data from the Lowell Photometric Database and from the Wide-field Infrared Survey Explorer (WISE) was published in 2018. It gave a concurring sidereal period of hours and includes a partial spin axis at (β1 −53.0°) in ecliptic coordinates (λ, β). Diameter and albedo According to the survey carried out by the Infrared Astronomical Satellite IRAS, the Japanese Akari satellite, and the NEOWISE mission of NASA's WISE telescope, Ilsebill measures (), () and () kilometers in diameter and its surface has a low albedo of (), () and (), respectively. The Collaborative Asteroid Lightcurve Link derives its estimate from IRAS, that is, an albedo of 0.0638 and a diameter of 27.62 km based on an absolute magnitude of 11.4. Further published mean-diameters by the WISE team include (), (), (), () and () with albedos between () and (). References External links Lightcurve Database Query (LCDB), at www.minorplanet.info Dictionary of Minor Planet Names, Google books Discovery Circumstances: Numbered Minor Planets (1)-(5000) – Minor Planet Center 000919 Discoveries by Max Wolf Named minor planets Grimms' Fairy Tales 000919 19181030

3037127

https://en.wikipedia.org/wiki/920%20Rogeria

920 Rogeria

920 Rogeria (prov. designation: or ) is a dark background asteroid from the central region of the asteroid belt, discovered by German astronomer Karl Reinmuth at the Heidelberg-Königstuhl State Observatory on 1 September 1919. The D-type asteroid (DT) has a rotation period of 12.2 hours and measures approximately in diameter. It was named "Rogeria", a name unrelated to the discoverer's contemporaries, that was taken from the almanac Lahrer Hinkender Bote. Orbit and classification Rogeria, located in the orbital region of the Eunomia family, is a non-family asteroid of the main belt's background population when applying the hierarchical clustering method to its proper orbital elements. It orbits the Sun in the central asteroid belt at a distance of 2.3–2.9 AU once every 4 years and 3 months (1,552 days; semi-major axis of 2.62 AU). Its orbit has an eccentricity of 0.11 and an inclination of 12° with respect to the ecliptic. The body's observation arc begins at Heidelberg Observatory with its official discovery observation. Naming This minor planet was named after the feminine form of the name "Roger", picked from the Lahrer Hinkender Bote, which was published in Lahr, southern Germany. A Hinkender Bote (lit. "limping messenger") was a very popular almanac, especially in the alemannic-speaking region from the late 17th throughout the early 20th century. The calendar section contains feast days, the dates of important fairs and astronomical ephemerides. For 5 January, the calendar gives "Roger" as the German name day analogue next to Simeon and Telesph., the protestant and catholic entries in the calendar of saints, likely referring to Simeon Stylites and Pope Telesphorus. Reinmuth's calendar names As with 22 other asteroids – starting with 913 Otila, and ending with 1144 Oda – Reinmuth selected names from this calendar due to his many asteroid discoveries that he had trouble thinking of proper names. These names are not related to the discoverer's contemporaries. Lutz Schmadel, the author of the Dictionary of Minor Planet Names learned about Reinmuth's source of inspiration from private communications with Dutch astronomer Ingrid van Houten-Groeneveld, who worked as a young astronomer at Heidelberg. Physical characteristics In the Tholen classification, Rogeria is closest to a dark D-type and somewhat similar to an uncommon T-type asteroid, though with an unusual spectrum (DTU). D-type asteroids are more common further out the asteroid belt and among the Jupiter trojan population. In the SDSS-based taxonomy, Rogeria is an X-type asteroid. Rotation period and poles In October 2010, a rotational lightcurve of Rogeria was obtained from photometric observations by Thomas A. Polakis at the Command Module Observatory in Arizona. Lightcurve analysis gave a rotation period of hours with a brightness variation of magnitude (). A tentative period determination of hours with an amplitude of magnitude was made by French amateur French astronomer René Roy in July 2012 (). Another observation by Petr Pravec and Peter Kušnirák at Ondřejov Observatory in June 2007 gave a period of 8.09 hours (). In 2016, a modeled lightcurve gave a concurring sidereal period of hours using data from the Uppsala Asteroid Photometric Catalogue, the Palomar Transient Factory survey, and individual observers (such as above), as well as sparse-in-time photometry from the NOFS, the Catalina Sky Survey, and the La Palma surveys . The study also determined two spin axes of (238.0°, −15.0°) and (47.0°, −35.0°) in ecliptic coordinates (λ, β). Diameter and albedo According to the survey carried out by the Infrared Astronomical Satellite IRAS, the Japanese Akari satellite, and the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer (WISE), Rogeria measures (), () and () kilometers in diameter and its surface has a low albedo of (), () and (), respectively. The Collaborative Asteroid Lightcurve Link derives an albedo of 0.0613 and a diameter of 29.71 km based on an absolute magnitude of 11.285. Further published mean-diameters and albedos by the WISE team include (), () and () with corresponding albedos of (), () and (). Notes References External links Lightcurve Database Query (LCDB), at www.minorplanet.info Dictionary of Minor Planet Names, Google books Asteroids and comets rotation curves, CdR – Geneva Observatory, Raoul Behrend Discovery Circumstances: Numbered Minor Planets (1)-(5000) – Minor Planet Center 000920 Discoveries by Karl Wilhelm Reinmuth Named minor planets 000920 19190901

3037131

https://en.wikipedia.org/wiki/921%20Jovita

921 Jovita

921 Jovita (prov. designation: or ) is a dark background asteroid, approximately in diameter, located in the outer regions of the asteroid belt. It was discovered on 4 September 1919, by astronomer Karl Reinmuth at the Heidelberg-Königstuhl State Observatory in southwest Germany. The carbonaceous C-type asteroid (Ch) has a rotation period of 15.6 hours and is likely spherical in shape. It was named "Jovita", a common German female name unrelated to the discoverer's contemporaries, that was taken from the almanac Lahrer Hinkender Bote. Orbit and classification Jovita is a non-family asteroid of the main belt's background population when applying the hierarchical clustering method to its proper orbital elements. It orbits the Sun in the outer asteroid belt at a distance of 2.6–3.8 AU once every 5 years and 8 months (2,061 days; semi-major axis of 3.17 AU). Its orbit has an eccentricity of 0.18 and an inclination of 16° with respect to the ecliptic. The body's observation arc begins at Heidelberg Observatory on 4 September 1919, the night after its official discovery observation. Naming This minor planet was named "Jovita", after a female name picked from the Lahrer Hinkender Bote, published in Lahr, southern Germany. A Hinkender Bote (lit. "limping messenger") was a very popular almanac, especially in the alemannic-speaking region from the late 17th throughout the early 20th century. The calendar section contains feast days, the dates of important fairs and astronomical ephemerides. The German name day analogue is given next to the protestant and catholic feast days (entry not found). Reinmuth's calendar names As with 22 other asteroids – starting with 913 Otila, and ending with 1144 Oda – Reinmuth selected names from this calendar due to his many asteroid discoveries that he had trouble thinking of proper names. These names are not related to the discoverer's contemporaries. Lutz Schmadel, the author of the Dictionary of Minor Planet Names learned about Reinmuth's source of inspiration from private communications with Dutch astronomer Ingrid van Houten-Groeneveld, who worked as a young astronomer at Heidelberg. Physical characteristics In the Tholen- and SMASS-like taxonomy of the Small Solar System Objects Spectroscopic Survey (S3OS2), Jovita is a hydrated, carbonaceous Caa and Ch-type asteroid, respectively. Rotation period In August 2004, a rotational lightcurve of Jovita was obtained from photometric observations by . Lightcurve analysis gave a rotation period of hours with a brightness variation of magnitude, indicative of a rather spherical shape (). A lower rated period determination of hours with an amplitude of magnitude was made by French amateur astronomers René Roy and Laurent Bernasconi in September 2004 (). Diameter and albedo According to the survey carried out by the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer (WISE), the Infrared Astronomical Satellite IRAS, and the Japanese Akari satellite, Jovita measures (), () and () kilometers in diameter and its surface has a low albedo of (), () and (), respectively. The Collaborative Asteroid Lightcurve Link assumes an albedo of 0.0670 and a diameter of 58.95 km based on an absolute magnitude of 9.7. Alternative mean-diameters published by the WISE team include (), (), () and () with albedos between 0.048 and 0.069. An asteroid occultation, observed on 5 February 2007, gave a best-fit ellipse dimension of 58.0 × 58.0 kilometers. These timed observations are taken when the asteroid passes in front of a distant star. However the quality of the measurement is rated poorly. Notes References External links Lightcurve Database Query (LCDB), at www.minorplanet.info Dictionary of Minor Planet Names, Google books Asteroids and comets rotation curves, CdR – Geneva Observatory, Raoul Behrend Discovery Circumstances: Numbered Minor Planets (1)-(5000) – Minor Planet Center 000921 Discoveries by Karl Wilhelm Reinmuth Named minor planets 19190904

3037136

https://en.wikipedia.org/wiki/923%20Herluga

923 Herluga

923 Herluga (prov. designation: or ) is a three-body resonant background asteroid, approximately in diameter, located in the central region of the asteroid belt. It was discovered on 30 September 1919, by astronomer Karl Reinmuth at the Heidelberg Observatory in southwest Germany. The carbonaceous C-type asteroid has a rotation period of 19.7 hours. It was named "Herluga", a common German female name unrelated to the discoverer's contemporaries, that was taken from the almanac Lahrer Hinkender Bote. Orbit and classification Herluga is a non-family asteroid of the main belt's background population when applying the hierarchical clustering method to its proper orbital elements. Located in the orbital region of the Eunomia family, Herluga orbits the Sun in the central asteroid belt at a distance of 2.1–3.1 AU once every 4 years and 3 months (1,546 days; semi-major axis of 2.62 AU). Its orbit has an eccentricity of 0.19 and an inclination of 14° with respect to the ecliptic. This brings the object into a pure three-body resonance (2/2/-1) with Jupiter and Saturn (ares 2.615 AU). Other asteroids in this resonant group of 34 known objects include 70 Panopaea, 194 Prokne, 258 Tyche, 839 Valborg and 995 Sternberga. Herluga was first observed as () at Simeiz Observatory on the Crimean peninsula on 9 November 1915. The body's observation arc begins at Heidelberg Observatory on 10 December 1919, more than two months after its official discovery observation. Naming This minor planet was named "Herluga", after a female name picked from the Lahrer Hinkender Bote, published in Lahr, southern Germany. A Hinkender Bote (lit. "limping messenger") was a very popular almanac, especially in the alemannic-speaking region from the late 17th throughout the early 20th century. The calendar section contains feast days, the dates of important fairs and astronomical ephemerides. For 2 March, the calendar gives "Herluga" as the German name day analogue next to Simplizius and Luise, the protestant and catholic entries in the calendar of saints. Reinmuth's calendar names As with 22 other asteroids – starting with 913 Otila, and ending with 1144 Oda – Reinmuth selected names from this calendar due to his many asteroid discoveries that he had trouble thinking of proper names. These names are not related to the discoverer's contemporaries. Lutz Schmadel, the author of the Dictionary of Minor Planet Names learned about Reinmuth's source of inspiration from private communications with Dutch astronomer Ingrid van Houten-Groeneveld, who worked as a young astronomer at Heidelberg. Physical characteristics In both the Tholen- and SMASS-like taxonomy of the Small Solar System Objects Spectroscopic Survey (S3OS2), Herluga is a common, carbonaceous C-type asteroid. Rotation period In November 2008, a rotational lightcurve of Herluga was obtained from photometric observations by James W. Brinsfield at the Via Capote Observatory in California. Lightcurve analysis gave a rotation period of hours with a brightness variation of magnitude (). In August 2016, an alternative period determination of hours with an amplitude of mag was published (). Diameter and albedo According to the survey carried out by the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer (WISE), the Japanese Akari satellite, and the Infrared Astronomical Satellite IRAS, Herluga measures (), () and () kilometers in diameter and its surface has a low albedo of (), () and (), respectively. The Collaborative Asteroid Lightcurve Link adopts the results obtained by IRAS, that is, an albedo of 0.0421 and a diameter of 32.47 km based on an absolute magnitude of 11.5. Further published mean-diameters by the WISE team in ascending order include (), (), (), () and () with albedos between 0.03 and 0.06. References External links Lightcurve Database Query (LCDB), at www.minorplanet.info Dictionary of Minor Planet Names, Google books Discovery Circumstances: Numbered Minor Planets (1)-(5000) – Minor Planet Center 000923 Discoveries by Karl Wilhelm Reinmuth Named minor planets 19190930