Datasets:

mattany

/

wikipedia-solarsystem

like 0

3033332

https://en.wikipedia.org/wiki/723%20Hammonia

723 Hammonia

723 Hammonia is a minor planet orbiting the Sun. It was discovered in 1911 and is named after the city of Hamburg. Although the name alludes to Hamburg it was discovered in Vienna. (Vienna is the capital of Austria) The asteroid was discovered by the noted and prolific astronomer Johann Palisa. He worked from Pola early in his career and later from Vienna observatories. The same night he discovered Hammonia, he also discovered 724 Hapag and 725 Amanda. He discovered dozens and dozens of asteroids between 1874 and 1923, ranging from 136 Austria to 1073 Gellivara. As seen from a certain area on Earth, 723 Hammonia occulted the star 3UC149-190572 on June 3, 2013. In 2014 it was noted to have a high-albedo and amorphous Mg pyroxenes was suggested as a possible reason for this. See also 449 Hamburga (another asteroid named after Hamburg) Vienna Observatory References External links Background asteroids Hammonia Hammonia C-type asteroids (SMASS) 19111021

3033334

https://en.wikipedia.org/wiki/724%20Hapag

724 Hapag

724 Hapag is a minor planet orbiting the Sun in the asteroid belt that was found by Austrian astronomer Johann Palisa in 1911 and named after the German shipping company Hamburg America Line. It was assigned a provisional name of 1911 NC, then became a lost asteroid until it was rediscovered in 1988 as by Tsutomu Hioki and N. Kawasato at Okutama, Japan. 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 3.1305 ± 0.0001 hours and a brightness variation of 0.11 ± 0.01 in magnitude. References External links Background asteroids 19111021 Hapag Hapag

3033338

https://en.wikipedia.org/wiki/726%20Jo%C3%ABlla

726 Joëlla

726 Joëlla is a minor planet orbiting the Sun. It was discovered on November 22, 1911, by Joel Hastings Metcalf, in Winchester, Massachusetts, in the United States. References External links Background asteroids Joella 19111122 Joella

3033339

https://en.wikipedia.org/wiki/727%20Nipponia

727 Nipponia

727 Nipponia is a minor planet orbiting the Sun. It is a member of the Maria family of asteroids. Nipponia was originally discovered by Shin Hirayama in Tokyo on March 6, 1900. However, he was not able to determine its orbit. After it was rediscovered by Adam Massinger on February 11, 1912, Massinger gave the honor of naming it to Hirayama, who chose to name it from a latinization of "Nippon" (Japan in Japanese). Massinger, however, remains the officially credited discoverer of Nipponia. References External links Maria asteroids Nipponia Nipponia Nipponia DT-type asteroids (Tholen) 19120211

3033341

https://en.wikipedia.org/wiki/728%20Leonisis

728 Leonisis

728 Leonisis is an asteroid of the Flora family, discovered by Austrian astronomer Johann Palisa on 16 February 1912 from Vienna. There is some uncertainty as to its spectral class. It has been previously placed in the rare A and Ld classes. These are generally "stony" spectra, but with significant deviations from the usual S-type. The unusual spectrum brings Leonisis' membership in the Flora family into doubt. Photometric observations of this asteroid from the Organ Mesa Observatory in Las Cruces, New Mexico, during 2010 gave a light curve with a period of 5.5783 ± 0.0002 hours and a brightness variation of 0.20 ± 0.04 magnitude. References External links Flora asteroids Leonisis 19120216 Leonisis

3033342

https://en.wikipedia.org/wiki/729%20Watsonia

729 Watsonia

729 Watsonia is a rare-type asteroid and namesake of the Watsonia family from the central region of the asteroid belt. It was named after the Canadian-American astronomer James C. Watson. Watsonia occulted the star 54 Leonis (HIP 53417, a 4.3 Magnitude Star) on 2013 Mar 03 at 01:48. Description This object is the namesake of the Watsonia family, an Asteroid family of approximately 100 asteroids that share similar spectral properties and orbital elements; hence they may have arisen from the same collisional event. All members have a relatively high orbital inclination. References External links Watsonia asteroids Watsonia Watsonia STGD-type asteroids (Tholen) L-type asteroids (SMASS) 19120209

3033345

https://en.wikipedia.org/wiki/731%20Sorga

731 Sorga

731 Sorga (prov. designation: or ) is a highly elongated background asteroid from the outer regions of the asteroid belt, approximately in diameter. It was discovered on 15 April 1912, by German astronomer Adam Massinger at the Heidelberg-Königstuhl State Observatory in southwest Germany. The C-type (CD) and X-type asteroid (Xe) has a rotation period of 8.2 hours. It was named Sorga, meaning "the heavens" in the Indonesian language. Orbit and classification Sorga 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 (1,886 days; semi-major axis of 2.99 AU). Its orbit has an eccentricity of 0.14 and an inclination of 11° with respect to the ecliptic. The body's observation arc begins at Heidelberg Observatory on 21 October 1919, more than seven years after its official discovery observation. Naming This minor planet was named Sorga, the word for "the heavens" in the Indonesian language, also transliterated as "surga". The was not mentioned in The Names of the Minor Planets by Paul Herget. Physical characteristics In the Tholen classification, Sorga is closest to a common, carbonaceous C-type asteroid and somewhat similar to a dark D-type asteroid (CD), while in the Bus–Binzel SMASS classification, it is an Xe-subtype which transitions from the X-type to the bright E-type. Sorga has also been classified as a metallic M-type asteroid. Rotation period and poles In April 2005, a rotational lightcurve of Sorga was obtained from photometric observations by Brian Warner at his Palmer Divide Observatory in Colorado. Analysis gave a classically shaped bimodal lightcurve with a well-defined rotation period of () hours and a high brightness variation of () magnitude, indicative of its elongated shape (). In February 2009, Warner revisited Sorga and determined a very similar period of () hours though with a much lower amplitude of () magnitude (). In January 2010, astronomers at the Palomar Transient Factory measured a period of hours with an amplitude of magnitude (). Additional observations by Christophe Demeautis in September 2017, and by Bruno Christmann in April 2020, gave a period of () and () hours with an amplitude of and magnitude, respectively (). In 2016, a modeled lightcurve rendered a concurring sidereal period of hours using data from the Uppsala Asteroid Photometric Catalogue, the Palomar Transient Factory survey, and individual observers, 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 (83.0°, 40.0°) and (275.0°, 21.0°) 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, Sorga measures (), () and () kilometers in diameter and its surface has an albedo of (), () and (), respectively. The Collaborative Asteroid Lightcurve Link derives an albedo of 0.1339 and a diameter of 41.70 kilometers based on an absolute magnitude of 9.7. The WISE team also published an alternative mean-diameter of () with an albedo of (). Two asteroid occultations on 24 October 2007, and on 31 October 2012, gave a best-fit ellipse dimension of () and (), with an intermediate and low quality rating of 2 and 1, 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 Asteroids and comets rotation curves, CdR – Geneva Observatory, Raoul Behrend Discovery Circumstances: Numbered Minor Planets (1)-(5000) – Minor Planet Center 000731 Discoveries by Adam Massinger Named minor planets 000731 000731 19120415

3033346

https://en.wikipedia.org/wiki/732%20Tjilaki

732 Tjilaki

732 Tjilaki (prov. designation: or ) is a dark background asteroid, approximately in diameter, located in the inner region of the asteroid belt. It was discovered by German astronomer Adam Massinger at the Heidelberg Observatory on 15 April 1912, and later named after the Cilaki (Tjilaki) river in Indonesia. The dark D-type asteroid has a rotation period of 12.3 hours. It was an early candidate to be visited by the Rosetta spacecraft which eventually rendezvoused comet 67P/Churyumov–Gerasimenko. Orbit and classification Tjilaki 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 2.3–2.6 AU once every 3 years and 10 months (1,406 days; semi-major axis of 2.46 AU). Its orbit has an eccentricity of 0.04 and an inclination of 11° with respect to the ecliptic. The body's observation arc begins at Heidelberg Observatory on 28 August 1913, or 16 months after its official discovery observation. Naming This minor planet was named after the Cilaki (Tjilaki) river in West Java, Indonesia. The river rises in the mountains where the city of Malabar (see asteroid 754 Malabar) is located. The was mentioned in The Names of the Minor Planets by Paul Herget in 1955 (). Rosetta mission In the Phase A study of the Rosetta mission, Tjilaki was considered an alternative visiting target to comet 46P/Wirtanen. However, both candidates were later abandoned in favor of comet 67P/Churyumov–Gerasimenko, which was visited by Rosetta in 2014. The retargeting was necessary as the spacecraft's launch window changed due to a delay caused by the launch failure of the satellite on the maiden flight of the Ariane 5 ECA carrier rocket in 2002. Physical characteristics In both the Tholen- and SMASS-like taxonomic variants of the Small Solar System Objects Spectroscopic Survey (S3OS2), , Tjilaki is a dark D-type asteroid, uncommon in the inner but abundant in the outer asteroid belt as well as among the Jupiter trojan population. Polarimetric observations also determined a D-type. Rotation period and poles In February 1996, a rotational lightcurve of Tjilaki was obtained from photometric observations over ten nights by European astronomers using the Dutch 0.9-metre Telescope and the Bochum 0.61-metre Telescope at La Silla Observatory in Chile. Lightcurve analysis gave a rotation period of hours with a brightness variation of magnitude (). In May 2012, astronomers at the Palomar Transient Factory measured a period of hours (). Additional observations were made by the TESS-team in January 2019, and by amateur astronomers Axel Martin and Rui Goncalves in May 2020, reporting a concurring period of () and () hours with an amplitude of () and () magnitude, respectively (). 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, 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 (160.0°, 23.0°) and (353.0°, 24.0°) 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, Tjilaki measures (), () and () kilometers in diameter and its surface has an albedo of (), () and (), respectively. The Collaborative Asteroid Lightcurve Link derives an albedo of 0.0763 and a diameter of 37.69 kilometers based on an absolute magnitude of 10.53. Alternative mean-diameters published by the WISE team include () and () with a corresponding albedo of () and (). Two asteroid occultations on 20 June 2005 and on 28 July 2009, gave a best-fit ellipse dimension of () and (), respectively, each with an intermediate quality rating of 2. 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 000732 Discoveries by Adam Massinger Named minor planets 19120415

3033348

https://en.wikipedia.org/wiki/733%20Mocia

733 Mocia

733 Mocia is a minor planet orbiting the Sun. A possible occultation was observed by Oscar Canales Moreno on October 1, 2001. See also List of minor planets/701–800 Meanings of minor planet names: 501–1000 References External links Cybele asteroids Mocia Mocia CF-type asteroids (Tholen) 19120916

3033349

https://en.wikipedia.org/wiki/730%20Athanasia

730 Athanasia

730 Athanasia (prov. designation: or ) is a background asteroid from the inner regions of the asteroid belt, approximately in diameter. It was discovered by Austrian astronomer Johann Palisa at the Vienna Observatory on 10 April 1912. The presumed stony S-type asteroid has a rotation period of 5.7 hours and is likely very elongated in shape. It was named Athanasia, the Greek word for "immortality". Orbit and classification Located in the region of the Flora family (), a giant asteroid family and the largest family of stony asteroids in the main-belt, Athanasia 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 4 months (1,228 days; semi-major axis of 2.24 AU). Its orbit has an eccentricity of 0.18 and an inclination of 4° with respect to the ecliptic. The body's observation arc begins at Vienna Observatory on 15 April 1912, or five nights after its official discovery observation. Naming This minor planet was named by friends of the discoverer after the Greek word for immortality, "athanasia". Any reference to a person or occurrence is unknown. The was mentioned in The Names of the Minor Planets by Paul Herget in 1955 (). Physical characteristics Athanasia is an assumed, stony S-type asteroid. Rotation period In February 2016, a rotational lightcurve of Athanasia was obtained from photometric observations by Frederick Pilcher at the Organ Mesa Observatory in New Mexico, United States. Analysis gave a classically shaped, well-defined bimodal lightcurve with a rotation period of hours and a very high brightness variation of magnitude, indicative of a highly elongated shape (). In May 2013, Pilcher already observed the object and reported a ambiguous period of or hours with an amplitude of magnitude (). Diameter and albedo According to the survey carried out by the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer, Athanasia measures () kilometers in diameter and its surface has a high albedo of (). The Collaborative Asteroid Lightcurve Link assumes a standard albedo for a Florian asteroid of 0.24 and calculates a diameter of 4.94 kilometers based on an absolute magnitude of 13.7. 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 000730 Discoveries by Johann Palisa Named minor planets 19120410

3033352

https://en.wikipedia.org/wiki/734%20Benda

734 Benda

734 Benda (prov. designation: or ) is a large background asteroid from the outer regions of the asteroid belt, approximately in diameter. It was discovered by Austrian astronomer Johann Palisa at the Vienna Observatory on 11 October 1912. For its size, the dark X-type asteroid has a relatively short rotation period of 7.1 hours. It was named after the discoverer's wife, Anna Benda. Orbit and classification Benda 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 2.8–3.5 AU once every 5 years and 7 months (2,040 days; semi-major axis of 3.15 AU). Its orbit has an eccentricity of 0.10 and an inclination of 6° with respect to the ecliptic. The body's observation arc begins at the discovering Vienna Observatory on 23 February 1920, almost eight years after its official discovery observation. Naming This minor planet was named by friends of the discoverer after Anna Benda, second wife of Johann Palisa, whom he married in 1902. However, the was erroneously attributed to the Czech composer Karel Bendl (1838–1897) in previous editions of the Dictionary of Minor Planet Names. Physical characteristics Benda is an X-type asteroid in both the Tholen- and SMASS-like taxonomic variants of the Small Solar System Objects Spectroscopic Survey (S3OS2). In agreement with its low albedo (see below), this object has also been classified as a C-type and P-type asteroid. Rotation period In October 2013, a rotational lightcurve of Benda was obtained from photometric observations over two nights by Robert Stephens at the Center for Solar System Studies in California. Lightcurve analysis gave a well-defined rotation period of hours with a brightness variation of magnitude (). In August 1995, a first period of hours was determined by Stefano Mottola (). In March 2004, French amateur astronomer René Roy obtained a period of hours with an amplitude of magnitude from three nights of observations (), while Robert K. Buchheim determined a period of hours and an amplitude of magnitude observing Benda over 10 nights at the Altimira Observatory in November 2007 (). In September 2018, a collaboration of the Italian Amateur Astronomers Union reported a period of hours with a brightness variation 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, Benda measures (), () and () kilometers in diameter and its surface has an albedo of (), () and (), respectively. The Collaborative Asteroid Lightcurve Link derives a low albedo of 0.0387 and a diameter of 70.71 kilometers based on an absolute magnitude of 9.9. Alternative mean-diameters published by the WISE team include (), (), (), () and () with a corresponding albedo of (), (), (), () and (). Two asteroid occultations on 4 April 2009 and on 3 September 2013, gave a best-fit ellipse dimension of () and (), respectively, each with a low quality rating of 1. 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 000734 Discoveries by Johann Palisa Named minor planets 19121011

3033354

https://en.wikipedia.org/wiki/735%20Marghanna

735 Marghanna

735 Marghanna (prov. designation: or ) is a large carbonaceous background asteroid from the central regions of the asteroid belt, approximately in diameter. It was discovered on 9 December 1912, by German astronomer Heinrich Vogt at the Heidelberg-Königstuhl State Observatory in southwest Germany. The dark C-type asteroid (Ch) has a rotation period of 20.6 hours and is rather regular in shape. It was named after Margarete Vogt and after Hanna, the mother and a relative of the discoverer, respectively. Orbit and classification Marghanna 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 1.9–3.6 AU once every 4 years and 6 months (1,647 days; semi-major axis of 2.73 AU). Its orbit has an eccentricity of 0.32 and an inclination of 17° with respect to the ecliptic. The body's observation arc begins at Heidelberg Observatory on 29 November 1921, almost nine years after its official discovery observation. Naming This minor planet was named by the discoverer Heinrich Vogt after his mother Margarete Vogt and after one of his relatives, Hanna. The was mentioned in The Names of the Minor Planets by Paul Herget in 1955 (). Physical characteristics In the Tholen classification and in the SDSS-based taxonomy, Marghanna is a common, carbonaceous C-type asteroid, while in the Bus–Binzel SMASS classification, it is a hydrated C-type (Ch). Rotation period In May 2011, a rotational lightcurve of Marghanna was obtained from photometric observations by American astronomer Brian Skiff and collaborators using telescopes at the Lowell Observatory in Flagstaff, Arizona. The 2019-revised lightcurve analysis gave a well-defined rotation period of () hours with a small brightness variation of () magnitude, indicative of a rather spherical shape (). Lower rated measurements determined a period of 15.95 hours (Rafa Mohamed, 1995), 24 hours (Raymond Poncy, 2005) and hours (Brian Skiff, 2014) with an amplitude of , and magnitude, respectively (). 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, Marghanna measures (), () and () kilometers in diameter and its surface has an albedo of (), () and (), respectively. The Collaborative Asteroid Lightcurve Link derives an albedo of 0.0423 and a diameter of 74.23 kilometers based on an absolute magnitude of 9.7, while the Cornell Mid-IR Asteroid Spectroscopy (MIDAS) survey determined a diameter of () kilometers and Benoit Carry one of () kilometers. Alternative mean-diameters published by the WISE team include (), (), () and () with a corresponding albedo of (), (), () and (). Two asteroid occultations on 11 March 2008 and on 4 May 2010, gave a best-fit ellipse dimension of () and (), respectively, each with an intermediate quality rating of 2. 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 000735 Discoveries by Heinrich Vogt Named minor planets 000735 000735 19121209

3033356

https://en.wikipedia.org/wiki/736%20Harvard

736 Harvard

736 Harvard (prov. designation: or ) is a stony background asteroid from the inner regions of the asteroid belt, approximately in diameter. It was discovered on 16 November 1912, by American astronomer Joel Hastings Metcalf at the Winchester Observatory . The bright S-type asteroid has a rotation period of 6.7 hours. It was named after Harvard University in Cambridge, Massachusetts. Orbit and classification Located in the orbital region of the Flora family (), Harvard 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 (1,193 days; semi-major axis of 2.2 AU). Its orbit has an eccentricity of 0.17 and an inclination of 4° with respect to the ecliptic. The body's observation arc begins at Heidelberg Observatory on 9 December 1912, or three weeks after its official discovery observation by Metcalf at Winchester. Naming This minor planet was named in honor of the prestigious Harvard University in Cambridge, Massachusetts, United States. The was also mentioned in The Names of the Minor Planets by Paul Herget in 1955 (). Physical characteristics In the Tholen classification, Harvard is a common, stony S-type asteroid. Rotation period In 1970s, a rotational lightcurve of Harvard was obtained from photometric observations by Ed Tedesco. Lightcurve analysis gave a well-defined rotation period of hours with a brightness variation of magnitude (). 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, Harvard measures (), () and () kilometers in diameter and its surface has an albedo of (), () and (), respectively. The Collaborative Asteroid Lightcurve Link derives an albedo of 0.2051 and a diameter of 16.89 kilometers based on an absolute magnitude of 11.2. An asteroid occultation observed on 25 May 2003, gave a best-fit ellipse dimension of () with a low quality rating of 1. 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 Discovery Circumstances: Numbered Minor Planets (1)-(5000) – Minor Planet Center 000736 Discoveries by Joel Hastings Metcalf Named minor planets 736 Harvard 000736 19121116

3033358

https://en.wikipedia.org/wiki/738%20Alagasta

738 Alagasta

738 Alagasta () is a main belt asteroid. It was discovered from Heidelberg on 7 January 1913 by German astronomer Franz Kaiser. The asteroid was named in honor of Gau-Algesheim, previously Alaghastesheim, which is the home city of the discoverer's family. This body is orbiting at a distance of with a period of and an eccentricity of 0.055. The orbital plane is inclined at an angle of 3.53° to the plane of the ecliptic. Photometric measurements made of the asteroid during 2015 produced a light curve that showed a rotation period of with a brightness variation of 0.11 in magnitude. The asteroid is roughly 63 km in diameter and has a low albedo. See also List of minor planets/701–800 Meanings of minor planet names: 501–1000 References External links Background asteroids Alagasta Alagasta CGSU-type asteroids (Tholen) 19130107

3033359

https://en.wikipedia.org/wiki/739%20Mandeville

739 Mandeville

739 Mandeville is a minor planet located in the asteroid belt. Its absolute magnitude is 8.50. It was discovered on 7 February 1913 by Joel Hastings Metcalf in Winchester, Massachusetts, and assigned the provisional code 1913 QR. A later, duplicate discovery was assigned the code 1963 HE. The orbital characteristics are calculated from the epoch of 4 January 2010, at which time 739 Mandeville had an orbital period of 1656 days and an orbital axis of 2.74 AU with eccentricity 0.14. Thus, its minimum distance from the sun was 2.35 and its maximum was 3.13. Its orbital inclination was found to be 20.71°, and its mean anomaly 116.58°. See also List of minor planets/701–800 Meanings of minor planet names: 501–1000 References External links Background asteroids Mandeville Mandeville X-type asteroids (Tholen) X-type asteroids (SMASS) 19130207

3033361

https://en.wikipedia.org/wiki/740%20Cantabia

740 Cantabia

740 Cantabia is a minor planet orbiting the Sun. It was discovered on 10 February 1913 at Winchester, Massachusetts by American amateur astronomer J. H. Metcalf. Cantabia is a contraction of Cantabrigia, Latin for Cambridge, named in honor of Cambridge, Massachusetts. It is orbiting at a distance of with a period of and an eccentricity (ovalness) of 0.11. Between 2014 and 2021, 740 Cantabia has been observed to occult three stars. This asteroid shows an exceptionally slow rate of spin. Photometry observations from two independent teams during 2009 were combined to generate a light curve showing a rotation period of with a brightness variation of in magnitude. The spectrum is classified as type CX in the Tholen taxonomy. It spans a girth estimated at ~91 km. See also List of minor planets/701–800 Meanings of minor planet names: 501–1000 References External links Lightcurve plot of 740 Cantabia, Palmer Divide Observatory, B. D. Warner (2009) 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 Background asteroids Cantabia Cantabia CX-type asteroids (Tholen) 19130210

3033362

https://en.wikipedia.org/wiki/742%20Edisona

742 Edisona

742 Edisona is a minor planet, specifically an asteroid orbiting in the asteroid belt that was discovered by German astronomer Franz Kaiser on February 23, 1913. It was named for inventor Thomas Edison. This asteroid is orbiting with a period of and an eccentricity of 0.119. The orbital plane is inclined at an angle of 11.2° to the plane of the ecliptic. 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. Photometric observations made during 2008 were used to produce a light curve of 742 Edisona showing a rotation period of with a brightness variation of in magnitude. It spans a girth of approximately 45.6 km. References External links Eos asteroids Edisona Edisona S-type asteroids (Tholen) K-type asteroids (SMASS) 19130223

3033363

https://en.wikipedia.org/wiki/741%20Botolphia

741 Botolphia

741 Botolphia is a 29.6-km diameter minor planet (specifically an asteroid) orbiting in the asteroid belt, discovered by American astronomer Joel Hastings Metcalf on 10 February 1913 from Winchester. It is named after Saint Botolph, the semi-legendary founder of a 7th-century monastery that would become the town of Boston, Lincolnshire, England. This asteroid is orbiting at a distance of from the Sun, with an orbital period of and an eccentricity (ovalness) of 0.07. The orbital plane is inclined at an angle of 8.41° to the ecliptic. Photometric data collected during 2007 were used to produce an asteroid light curve showing a rotation period of , with a brightness amplitude of 0.015 in magnitude. This result is consistent with earlier results by independent observers. 741 Botolphia was initially classified as an X-type asteroid, but it may instead belong to the M-type taxonomy. References External links Background asteroids Botolphia Botolphia X-type asteroids (Tholen) X-type asteroids (SMASS) 19130210

3033365

https://en.wikipedia.org/wiki/744%20Aguntina

744 Aguntina

744 Aguntina, provisional designation 1913 QW, is a rare-type carbonaceous asteroid from the outer region of the asteroid belt, about 60 kilometers in diameter. It was discovered by Austrian astronomer Joseph Rheden at Vienna Observatory, Austria, on 26 February 1913. The dark F-type asteroid, classified as a FX-subtype in the Tholen taxonomic scheme, orbits the Sun at a distance of 2.8–3.5 AU once every 5 years and 8 months (2,062 days). Its orbit is tilted by 8 degrees to the plane of the ecliptic and shows an eccentricity of 0.12. Photometric observations during 2003 showed a rotation period of hours with a brightness variation of in magnitude. The period has since been confirmed by an additional observation. According to the surveys carried out by the Infrared Astronomical Satellite, IRAS, the Japanese Akari satellite, and the U.S. Wide-field Infrared Survey Explorer with its subsequent NEOWISE mission, the asteroid's surface has a very low albedo between 0.03 and 0.05 and a diameter estimate that varies between 55 and 68 kilometers. The minor planet was named for the ancient Roman town, Aguntum, in the Noricum province of the Roman Empire, in what is nowadays mostly Austria. The naming information was given by the discoverer's widow, who was also the daughter of prolific astronomer Johann Palisa. The historic ruins are located close to Lienz in East Tyrol, the home town of the discoverer. In 1912, shortly before the minor planet's discovery, extensive excavations took place at the Roman site which unearthed coins, pottery masks, bronze objects, and painted tombstones. 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 Background asteroids Aguntina Aguntina FX:-type asteroids (Tholen) 19130226

3033366

https://en.wikipedia.org/wiki/743%20Eugenisis

743 Eugenisis

743 Eugenisis is a minor planet orbiting the Sun that was discovered by German astronomer Franz Kaiser in 1913. Photometric observations of this asteroid collected during 2004 show a rotation period of 10.23 ± 0.01 hours with a brightness variation of 0.20 ± 0.02 magnitude. The spectrum of this object matches the Ch class in the SMASS taxonomy, indicating a carbonaceous surface with a hydrous component. References External links Background asteroids Eugenisis Eugenisis Ch-type asteroids (SMASS) 19130225

3033368

https://en.wikipedia.org/wiki/745%20Mauritia

745 Mauritia

745 Mauritia (prov. designation: or ) is a dark background asteroid from the outer regions of the asteroid belt, approximately in diameter. It was discovered on 1 March 1913, by German astronomer Franz Kaiser at the Heidelberg-Königstuhl State Observatory in Germany. The presumed carbonaceous C-type asteroid has a rotation period of 9.9 hours. It was named after Saint Maurice, patron of the Saint Mauritius church in the city of Wiesbaden, where the discoverer was born. Orbit and classification Mauritia 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 3.1–3.4 AU once every 5 years and 11 months (2,154 days; semi-major axis of 3.26 AU). Its orbit has an eccentricity of 0.04 and an inclination of 13° with respect to the ecliptic. The body's observation arc begins at Heidelberg on 3 January 1918, almost five years after its official discovery observation. Naming This minor planet was named after 3rd-century Christian martyr Saint Maurice, who is the patron of the church in Wiesbaden, Germany, where the discoverer was born (also see 717 Wisibada). The Swiss village Saint-Maurice, where he died in AD 287 is also named after Saint Maurice. The was mentioned in The Names of the Minor Planets by Paul Herget in 1955 (). Physical characteristics Mauritia is an assumed, carbonaceous C-type asteroid due to its low albedo (see below) and its location in the outer asteroid belt. However, D-type and P-type asteroids fulfill the location and albedo-based criterions as well. Rotation period In March 2013, a first rotational lightcurve of Mauritia was obtained from photometric observations over six nights by Frederick Pilcher at the Organ Mesa Observatory in New Mexico, United States. Lightcurve analysis gave a well-defined rotation period of hours with a brightness variation of magnitude (). 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), Mauritia 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 44.22 kilometers based on an absolute magnitude of 10.5. The WISE team also published an alternative mean-diameter of () with an albedo of (). 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 000745 Discoveries by Franz Kaiser Named minor planets 19130301

3033370

https://en.wikipedia.org/wiki/746%20Marlu

746 Marlu

746 Marlu (prov. designation: or ) is a dark and large background asteroid from the outer regions of the asteroid belt, approximately in diameter. It was discovered on 1 March 1913, by German astronomer Franz Kaiser at the Heidelberg Observatory in southwest Germany. The primitive P-type asteroid has a rotation period of 7.8 hours. It was named after the discoverer's daughter, Marie-Louise Kaiser. Orbit and classification Marlu 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 2.4–3.8 AU once every 5 years and 6 months (2,003 days; semi-major axis of 3.11 AU). Its orbit has an eccentricity of 0.24 and an inclination of 17° with respect to the ecliptic. The body's observation arc begins at Heidelberg on 12 September 1915, more than two years after its official discovery observation. Naming Franz Kaiser named this minor planet after his daughter, the physician Marie-Louise Kaiser. The discoverer also named another asteroid, 743 Eugenisis, in honor of his daughter. The was mentioned in The Names of the Minor Planets by Paul Herget in 1955 (). Physical characteristics In the Tholen classification, Marlu is a dark and primitive P-type asteroid, while it is an X-type and P-type asteroid, in the Tholen- and SMASS-like taxonomic variant of the Small Solar System Objects Spectroscopic Survey (S3OS2), respectively. P-type asteroids are common in the outer asteroid belt and among the Jupiter trojan population. In the Moving Object Catalog (MOC) of the Sloan Digital Sky Survey, however, Marlu is a common carbonaceous C-type asteroid. Rotation period and poles In September 1981, a rotational lightcurve of Marlu was obtained from photometric observations by American astronomer Alan W. Harris. Lightcurve analysis gave a rotation period of hours with a brightness variation of magnitude (). In October 2014, Daniel A. Klinglesmith confirmed the exact same period of () hours with an amplitude of () magnitude (). In 2016, a modeled lightcurve gave a concurring sidereal period of hours using data from a large collaboration of individual observers. The study also determined two spin axes of (202.0°, −66.0°) and (64.0°, −27.0°) 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), Marlu measures (), () and () kilometers in diameter and its surface has a low albedo of ), () and (), respectively. The Collaborative Asteroid Lightcurve Link adopts an albedo of 0.0431 and derives a diameter of 69.87 kilometers based on an absolute magnitude of 9.81. The WISE-team also published two alternative mean-diameters of () and () with a corresponding albedo of () and (). An asteroid occultation on 1 May 1985, gave a best-fit ellipse dimension of () with an intermediate quality rating of 2. 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 Discovery Circumstances: Numbered Minor Planets (1)-(5000) – Minor Planet Center 000746 Discoveries by Franz Kaiser Named minor planets 000746 19130301

3033372

https://en.wikipedia.org/wiki/747%20Winchester

747 Winchester

747 Winchester is an asteroid, a minor planet orbiting the Sun. It was discovered in 1913, and is named after the town in which it was discovered, Winchester, Massachusetts, in the USA. Photometric observations of this asteroid at the Palmer Divide Observatory in Colorado Springs, Colorado in 2007 gave a light curve with a period of 9.4146 ± 0.0002 hours and a brightness variation of 0.16 ± 0.02 in magnitude. This is reasonably consistent with independent results reported in 1983 (9.40h), 1993 (9.402h), and 2007 (9.334h). References External links Lightcurve plot of 747 Winchester, Palmer Divide Observatory, B. D. Warner (2007) 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 Background asteroids Winchester Winchester PC-type asteroids (Tholen) C-type asteroids (SMASS) 19130307

3033373

https://en.wikipedia.org/wiki/748%20Sime%C3%AFsa

748 Simeïsa

748 Simeïsa (prov. designation: or ) is a very large Hilda asteroid from the outermost regions of the asteroid belt, approximately in diameter. It was discovered on 14 March 1913, by Russian astronomer Grigory Neujmin at the Simeiz Observatory on the Crimean peninsula. The dark P-type asteroid has a rotation period of 11.9 hours and a shape that is reminiscent of a tetrahedron. It was the first asteroid discovery made in Russia and named after the discovering observatory and its nearby Crimean town, Simeiz. Orbit and classification Simeïsa is a member of the distant orbital Hilda group of asteroids, which stay in a 3:2 orbital resonance with the gas giant Jupiter. It is however not a member of the collisional Hilda family () but a non-family asteroid of the background population when applying the hierarchical clustering method to its proper orbital elements. It orbits the Sun in the outermost asteroid belt at a distance of 3.2–4.7 AU once every 7 years and 10 months (2,864 days; semi-major axis of 3.95 AU). Its orbit has an eccentricity of 0.19 and an inclination of 2° with respect to the ecliptic. The body's observation arc begins at the Heidelberg Observatory on 19 February 1920, almost 7 years after its official discovery observation by Grigory Neujmin at Simeiz. Naming This minor planet was named after the discovering Simeiz Observatory and its nearby Crimean town, Simeiz. Simeïsa was the first minor planet discovered in Russia. The was mentioned in The Names of the Minor Planets by Paul Herget in 1955 (). Physical characteristics In the Tholen classification, Simeïsa is a dark and primitive P-type asteroid, which are common in the outer regions of asteroid belt and among the Jupiter trojan population. In the SDSS-based taxonomy, it is an X-type asteroid. Rotation period In October 2011, a rotational lightcurve of Simeïsa was obtained from photometric observations by French amateur astronomer René Roy. Lightcurve analysis gave a rotation period of () hours with a brightness variation of () magnitude (). In the 1990s, Mats Dahlgren already determined a period of hours with an amplitude of magnitude (). 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, Simeïsa measures (), () and () kilometers in diameter and its surface has a low albedo of (), () and (), respectively. The Collaborative Asteroid Lightcurve Link assumes an albedo of 0.0376 and derives a diameter of 102.79 kilometers based on an absolute magnitude of 9.12. Alternative mean-diameter measurements published by the WISE team include () and () with corresponding albedos of () and (). Two asteroid occultations on 4 March 1999 and 7 January 2006, gave a best-fit ellipse dimension of () and (), respectively, each with a quality rating of 2. 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 000748 Discoveries by Grigory Neujmin Named minor planets 000748 19130314

3033374

https://en.wikipedia.org/wiki/749%20Malzovia

749 Malzovia

749 Malzovia (prov. designation: or ) is a stony background asteroid from the inner regions of the asteroid belt, approximately in diameter. It was discovered on 5 April 1913, by Russian astronomer Sergey Belyavsky at the Simeiz Observatory on the Crimean peninsula. The elongated S-type asteroid has a rotation period of 5.9 hours. It was named after Russian amateur astronomer Nikolai Maltsov (S. I. Maltsov) who founded the discovering Simeïs Observatory in 1900. Orbit and classification Located in the region of the Flora family (), a giant asteroid family and the largest family of stony asteroids, Malzovia 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 1.9–2.6 AU once every 3 years and 4 months (1,228 days; semi-major axis of 2.24 AU). Its orbit has an eccentricity of 0.17 and an inclination of 5° with respect to the ecliptic. The body's observation arc begins at the German Heidelberg Observatory on 30 April 1913, or 25 days after its official discovery observation at Simeiz Observatory. Naming This minor planet was named after Russian amateur astronomer Nikolai Sergeevich Maltsov (S. I. Malzov) who founded the discovering Simeiz Observatory, which he later donated to the Pulkovo Observatory in 1911. Malzov was a close friend of Sergey Belyavsky and of Oskar Backlund, after whom asteroid 856 Backlunda was named. After World War I, Malzov lived at Menton, on the French Riviera near Italy. The was mentioned in The Names of the Minor Planets by Paul Herget in 1955 (). Physical characteristics In the Tholen and Bus–Binzel SMASS classification, Malzovia is a common, stony S-type asteroid. Rotation period In February 2020, a rotational lightcurve of Malzovia 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 its elongated shape (). Alternative period determinations by Julian Oey and Frederick Pilcher in May 2014 gave very similar results of () and () hours, respectively, both with an amplitude of 0.30 magnitude (). Poles Published in 2018, thermophysical modeling of Malzovia from thermal data obtained from the Wide-field Infrared Survey Explorer (WISE) gave a sidereal period of () and two spin axes at (53.0°, 37.0°) and (242.0°, 46.0°) in ecliptic coordinates (λ, β). Previously, two lightcurves published in 2016, using modeled photometric data from the Lowell Photometric Database (LPD) and other sources, gave a period of () and hours, respectively. Each modeled lightcurve also determined two poles at (53.0°, 37.0°) and (242.0°, 46.0°), as well as (55.0°, 46.0°) and (246.0°, 55.0°), respectively. Diameter and albedo According to the surveys carried out by the Japanese Akari satellite and the NEOWISE mission of NASA's WISE telescope, Malzovia measures () and () kilometers in diameter and its surface has a low albedo of () and (), respectively. The Collaborative Asteroid Lightcurve Link assumes an albedo of 0.24 and calculates a diameter of 12.98 kilometers based on an absolute magnitude of 11.6. The WISE team also published several alternative mean-diameters of (), () and (), with a corresponding albedo 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 000749 Discoveries by Sergei Belyavsky Named minor planets 000749 000749 19130405

3033375

https://en.wikipedia.org/wiki/750%20Oskar

750 Oskar

750 Oskar is a minor planet, specifically an asteroid orbiting in the asteroid belt that was discovered by Johann Palisa on 28 April 1913 in Vienna. Photometric observations made in 2012 at the Organ Mesa Observatory in Las Cruces, New Mexico, produced a light curve with a period of 6.2584 ± 0.0002 hours and a brightness variation of 0.21 ± 0.02 in magnitude. This is a member of the Nysa family of asteroids that share similar orbital elements. References External links Nysa asteroids Oskar Oskar F-type asteroids (Tholen) 19130428

3033377

https://en.wikipedia.org/wiki/725%20Amanda

725 Amanda

725 Amanda (prov. designation: or ) is a dark background asteroid, approximately in diameter, that is located in the central regions of the asteroid belt. It was discovered by Austrian astronomer Johann Palisa at the Vienna Observatory on 21 October 1911. The carbonaceous C-type asteroid (CSU/C0) has a short rotation period of 3.7 hours. It was named after Amanda Schorr, wife of German astronomer Richard Schorr (1867–1951). Orbit and classification Amanda 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 2.0–3.1 AU once every 4 years and 2 months (1,507 days; semi-major axis of 2.57 AU). Its orbit has an eccentricity of 0.22 and an inclination of 4° with respect to the ecliptic. The body's observation arc begins at Vienna Observatory on 29 September 1915, almost four years after its official discovery observation. Naming This minor planet was named after Amanda Ruth Smith, born to John and Ruth Smith of Jackson, MS.(May 1980). Amanda(human) was named for the song "Amanda" by Waylon Jennings. Her mother always said that she chose that name because she, like the song verse was always "Amanda light of my life." In 2010, Ruth Smith made the first ever arrangement with NASA to legally purchase the minor planet, "Amanda U1911" for an undisclosed sum of money(USD) and exclusively owns all rights to it. Amanda Ruth Smith (human) was given a certified certificate of ownership by NASA with the serial number "SHMILY-12.0522."© Physical characteristics In the Tholen classification, Amandas spectral type is closest to that of a carbonaceous C-type asteroid, yet also somewhat similar to a stony S-type with an "unusual" spectrum (CSU). In the taxonomy by Barucci (1987), the asteroid is a dark C-type (C0). Rotation period and poles A rotational lightcurve of Amanda was obtained from photometric observations by European astronomers at the La Silla Observatory before 1995. Lightcurve analysis gave a well-defined rotation period of hours with a brightness variation of magnitude (). In October 2010, French amateur astronomer Maurice Audejean determined a concurring period of () hours with an amplitude of () magnitude (), while in August 2018, a further observation by the TESS-team reported a period of () hours and an amplitude of () magnitude (). 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, 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 (145.0°, −63.0°) and (320.0°, −70.0°) 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), Amanda measures (), () and () in diameter and its surface has an albedo of (), () and (), respectively. The Collaborative Asteroid Lightcurve Link derives an albedo of 0.0824 and calculates a diameter of 21.56 kilometers based on an absolute magnitude of 11.66. Alternative mean-diameters published by the WISE team include (), (), () and () with a corresponding albedo 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 000725 Discoveries by Johann Palisa Amanda 000725 19111021

3033378

https://en.wikipedia.org/wiki/737%20Arequipa

737 Arequipa

737 Arequipa is a minor planet orbiting the Sun. It was discovered by American astronomer Joel Hastings Metcalf on 7 December 1912 from Winchester, Massachusetts. This stony S-type asteroid was named after the Peruvian city of Arequipa, where Harvard's Boyden Observatory was located prior to 1927. It is orbiting at a distance of from the Sun, with an orbital eccentricity (ovalness) of 0.245 and a period of . The orbital plane is inclined at an angle of 12.4° to the ecliptic. The rotation period of this asteroid has proven to be a challenge to determine, most likely because it has a complex shape and a rotation axis with a low inclination. However, during the 2015 apparition, photometric measurements of the asteroid were taken from close to the equatorial perspective. The resulting light curve displayed a rotation period of . See also List of minor planets/701–800 Meanings of minor planet names: 501–1000 References External links Background asteroids Arequipa Arequipa S-type asteroids (Tholen) S-type asteroids (SMASS) 19121207

3033397

https://en.wikipedia.org/wiki/751%20Fa%C3%AFna

751 Faïna

751 Faïna (prov. designation: or ) is a very large background asteroid from the central regions of the asteroid belt, approximately in diameter. It was discovered on 28 April 1913, by Russian astronomer Grigory Neujmin at the Simeiz Observatory on the Crimean peninsula. The elongated C-type asteroid (Ch) has a rotation period of 23.7 hours. It was named after Faina Mikhajlovna Neujmina, colleague and first wife of the discoverer. Orbit and classification Located close to the region of the stony Eunomia family (), Faïna is a non-family asteroid of the main belt's background population when applying the modern synthetic hierarchical clustering method (HCM) by Nesvorný as well as Milani and Knežević (AstDys). However, in the 1995 HCM-analysis by Zappalà, Faïna is the parent body of the tiny Faïna family, which is not recognized by modern analysis. The HCM-method is based on an object's proper orbital elements to group asteroids into families. Faïna orbits the Sun in the central asteroid belt at a distance of 2.2–2.9 AU once every 4 years and 1 month (1,489 days; semi-major axis of 2.55 AU). Its orbit has an eccentricity of 0.15 and an inclination of 16° with respect to the ecliptic. The body's observation arc begins at Vienna Observatory on 8 May 2013, or two weeks after its official discovery observation by Grigory Neujmin at Simeiz. Naming This minor planet was named after Faina Mikhajlovna Neujmina, the first wife of the discoverer. Astronomer Lutz Schmadel compiled this , based on his private communication with "N. S. Samojlova-Yakhontova", as neither the Minor Planet Circulars nor The Names of the Minor Planets give any information about this asteroid's name. Physical characteristics In the Tholen classification, Faïna is a common, carbonaceous C-type asteroid, while in the Bus–Binzel SMASS classification, it is a hydrated carbonaceous Ch-type. Rotation period In late 1988, a rotational lightcurve of Faïna was obtained from photometric observations by Richard Miles at the Manley Observatory near Chester in northwest England. Lightcurve analysis gave a well-defined rotation period of hours with a brightness variation of magnitude (). Alternative observations by Roberto Crippa, Federico Manzini (2006) as well as by Bruno Christmann (2019) determined a period of + and () hours (or half the period) with an amplitude of and magnitude (). 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), Faïna measures (), () and () kilometers in diameter and its surface has a low albedo of (), () and (), respectively. The Collaborative Asteroid Lightcurve Link adopts the results from IRAS, that is, an albedo of 0.0497 and a diameter of 110.50 kilometers based on an absolute magnitude of 8.66. The WISE team also published several alternative mean-diameters of (), (), (), () and (), with a corresponding albedo of (), (), (), (), and (). On 28 March 2007, an asteroid occultation of Faïna gave a best-fit ellipse dimension of () with a quality rating of 2, indicating its irregular, elongated shape. Another occultation on 21 October 2012, gave an ellipse 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 000751 000751 Discoveries by Grigory Neujmin Named minor planets 000751 000751 19130428

3033404

https://en.wikipedia.org/wiki/752%20Sulamitis

752 Sulamitis

752 Sulamitis is an asteroid from the inner regions of the asteroid belt, approximately in diameter. It is the parent body of the Sulamitis family (), a small family of 300 known carbonaceous asteroids. This asteroid is orbiting from the Sun with a period of and an eccentricity of 0.0743. The orbital plane is inclined at an angle of 5.96° to the plane of the ecliptic. Sulamitis was discovered on 30 April 1913 by Georgian–Russian astronomer Grigory Neujmin at the Simeiz Observatory on the Crimean peninsula, and given the provisional designation . It was named after the Shulamite, a beautiful woman mentioned in the book Solomon's Song of Songs of the Old Testament. The figure is possibly the Queen of Sheba in the Hebrew Bible. Photometric observations of this asteroid collected during 2004–2005 show a rotation period of with a brightness variation of magnitude. A hydration feature in the spectrum of 752 Sulamitis indicates the surface has undergone aqueous alteration. The same feature appears in most of its family members, suggesting the original body held water in some form. References External links Discovery Circumstances: Numbered Minor Planets 000752 Discoveries by Grigory Neujmin Named minor planets 19130430

3033406

https://en.wikipedia.org/wiki/754%20Malabar

754 Malabar

754 Malabar is a minor planet orbiting the Sun. It was discovered in 1906 by German astronomer August Kopff from Heidelberg, and was named in honor of a Dutch-German solar eclipse expedition to Christmas Island in 1922. Malabar is the name of a city and mountain in Indonesia. This object is orbiting at a distance of from the Sun with a period of and an eccentricity (ovalness) of 0.048. Its orbital plane is inclined at an angle of 24.6° to the plane of the ecliptic. Photometric measurements of this asteroid made in 2003 resulted in a light curve showing a rotation period of and a brightness variation of in magnitude. This is a Ch-class asteroid in the Bus asteroid taxonomy, showing a broad absorption band in its carbonaceous spectrum near a wavelength of 0.7 μm. This feature is interpreted as due to iron-bearing phyllosilicates on the surface. 754 Malabar spans a girth of 102.8 km. Between 2002 and 2022, 754 Malabar has been observed to occult sixteen stars. References External links Background asteroids Malabar Malabar XC-type asteroids (Tholen) Ch-type asteroids (SMASS) 19060822

3033408

https://en.wikipedia.org/wiki/755%20Quintilla

755 Quintilla

755 Quintilla (prov. designation: or ) is a metallic background asteroid from the outer regions of the asteroid belt, approximately in diameter. It was discovered on 6 April 1908, by American astronomer Joel Metcalf at the Taunton Observatory in Massachusetts, United States. For its size, the M-type asteroid has a relatively short rotation period of 4.55 hours. It was named Quintilla, an Italian female first name, for no reason other than being the first asteroid name beginning with the letter "Q". Orbit and classification Quintilla 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 2.7–3.6 AU once every 5 years and 8 months (2,073 days; semi-major axis of 3.18 AU). Its orbit has an eccentricity of 0.14 and an inclination of 3° with respect to the ecliptic. The body's observation arc begins at Vienna Observatory on 1 September 1915, almost 7 years after its official discovery observation by Joel Metcalf at Taunton. Naming This minor planet was named Quintilla, a name of an Italian first name, that was proposed by Arville D. Walker, secretary to the American astronomer and director of Harvard Observatory Harlow Shapley (1885–1972), as no other asteroid name began with the letter "Q" when it was named in 1926. The was mentioned in The Names of the Minor Planets by Paul Herget in 1955 (). Physical characteristics In the Tholen classification, Quintilla is a metallic M-type asteroid. Rotation period Several rotational lightcurves of Quintilla were obtained from photometric observations. Analysis of the best-rated lightcurves by Robert K. Buchheim and Donald Pray (2004), Laurent Bernasconi, Reiner Stoss, Petra Korlević, Maja Hren, Aleksandar Cikota, Ljuban Jerosimic, and Raoul Behrend (2005), as well as Joseph Masiero (2006), gave a well-defined rotation period of (), () and () hours with a brightness variation of (), () and () magnitude, respectively (). In November 2018, Michael and Matthew Fauerbach obtained a period of () hours and an amplitude of () magnitude (). 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), Quintilla measures (), () and () kilometers in diameter and its surface has an albedo of (), () and (), respectively. Alternative mean-diameter measurements published by the WISE team include () and () with corresponding albedos of () and (). The Collaborative Asteroid Lightcurve Link derives an albedo of 0.1781 and a diameter of 36.16 kilometers based on an absolute magnitude of 9.7. 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 000755 Discoveries by Joel Hastings Metcalf Named minor planets 000755 19080406

3033411

https://en.wikipedia.org/wiki/756%20Lilliana

756 Lilliana

756 Lilliana is a minor planet orbiting the Sun that was discovered by American astronomer Joel Hastings Metcalf on 26 April 1908 from Taunton, Massachusetts. It rotates around its axis of rotation every 9.36 hours. Photometric observations of this asteroid at Palmer Divide Observatory in Colorado Springs, Colorado, during 2007 gave a light curve with a period of hours and a brightness variation of in magnitude. A 2012 study based upon observations at the Organ Mesa Observatory in Las Cruces, New Mexico, during 2012 produced a conflicting period of hours and a brightness variation of in magnitude. Further study will be needed to resolve the discrepancies in period and amplitude. References External links Lightcurve plot of 756 Lilliana, Palmer Divide Observatory, B. D. Warner (2007) 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 Background asteroids Lilliana 19080426 Lilliana

3033412

https://en.wikipedia.org/wiki/758%20Mancunia

758 Mancunia

758 Mancunia is a minor planet orbiting the Sun. It was discovered in 1912 from Johannesburg by H. E. Wood, a Mancunian. This object is orbiting at a distance of with a period of and an eccentricity (ovalness) of 0.15. The orbital plane is inclined at an angle of 5.61° to the plane of the ecliptic. Observation of this asteroid in 1996 suggested a rotation period of 6.902 hours. However, radar observations from Arecibo indicated this may be in error. Independent photometry measurements made during December 2006 were combined to determine an estimated period nearly double that of the original, or with a brightness variation amplitude of in magnitude. A high radar albedo indicates this object is most likely metallic. Dips in the radar echo suggests there are large concavities on both sides. It is classified as an X-type asteroid in the Tholen taxonomy and spans a girth of . References External links Lightcurve plot of 758 Mancunia, 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 Background asteroids Mancunia Mancunia X-type asteroids (Tholen) 19120518

3033413

https://en.wikipedia.org/wiki/757%20Portlandia

757 Portlandia

757 Portlandia is a main-belt asteroid 32 km in diameter. It was discovered on 30 September 1908 from Taunton, Massachusetts by the amateur American astronomer Joel E. Metcalf. The asteroid was named for the city of Portland, Maine, where Hastings was a church minister at the time. In November 2015, amateur astronomers captured it with images of comet 67P/Churyumov–Gerasimenko. Portlandia came to opposition in March 2016 at apparent magnitude 13.2. This body is orbiting at a distance of with a period of and an eccentricity of 0.109. The orbital plane is inclined at an angle of 8.2° to the plane of the ecliptic. 757 Portlandia is classified as an X-type asteroid and is a core member of the proposed Athor asteroid family, named after 161 Athor. This asteroid spans a girth of and is rotating with a period of 6.58 hours. During 2003, the asteroid was observed occulting a star. The resulting chords were used to determine a diameter estimate of 36.7 km. References External links Background asteroids Portlandia Portlandia XF-type asteroids (Tholen) Xk-type asteroids (SMASS) 19080930

3033416

https://en.wikipedia.org/wiki/759%20Vinifera

759 Vinifera

759 Vinifera (prov. designation: or ) is a large background asteroid from the central regions of the asteroid belt, approximately in diameter. It was discovered on 26 August 1913, by German astronomer Franz Kaiser at the Heidelberg-Königstuhl State Observatory in southwest Germany. The dark X-type asteroid has a rotation period of 14.2 hours and a heavily elongated shape. It was named after the plant species vitis vinifera, also known as the common grape vine. Orbit and classification Vinifera 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 (1,548 days; semi-major axis of 2.62 AU). Its orbit has an eccentricity of 0.21 and an inclination of 20° with respect to the ecliptic. The body's observation arc begins with its official discovery observation by Franz Kaiser at the Heidelberg Observatory on 26 August 1913. Naming This minor planet was named after the plant vitis vinifera, the common grape vine, to honor the discoverer's ancestors who were winemakers. The was mentioned in The Names of the Minor Planets by Paul Herget in 1955 (). Physical characteristics In the Bus–Binzel SMASS classification, Vinifera is an X-type asteroid. Rotation period In September 2002, a rotational lightcurve of Vinifera was obtained from photometric observations by Maurice Clark at the Goodsell Observatory in Minnesota. Lightcurve analysis gave a well-defined rotation period of hours with a brightness variation of magnitude (). Other observation by Jean-Gabriel Bosch, Jacques Michelet and René Roy (2002), Brian Uzpen and Steven Kipp (2002), as well as René Roy and Eric Barbotin (2019), gave nearly identical periods of , and hours with an amplitude of , and magnitude, respectively (). 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), Vinifera measures (), () and () kilometers in diameter and its surface has an albedo of (), () and (), respectively. Alternative mean-diameter measurements published by the WISE team include (), (), () and () with corresponding albedos of (), (), () and (). The Collaborative Asteroid Lightcurve Link derives an albedo of 0.0500 and a diameter of 45.07 kilometers based on an absolute magnitude of 10.6. On 13 January 2002, an asteroid occultation of Vinifera gave a best-fit ellipse dimension of (), with a quality rating of 2. Lower rated measurements on 3 October 2011 and on 20 November 2015, gave an 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 000759 Discoveries by Franz Kaiser Named minor planets 000759 19130826

3033419

https://en.wikipedia.org/wiki/753%20Tiflis

753 Tiflis

753 Tiflis is a minor planet orbiting the Sun. It was discovered 30 April 1913 by the Georgian–Russian astronomer Grigory N. Neujmin at Simeiz Observatory and was named after Georgia's capital city Tiflis (now called Tbilisi). The object is orbiting the Sun at a distance of with a period of and an eccentricity (ovalness) of 0.22. The orbital plane is inclined by an angle of 10.1° to the plane of the ecliptic. In 1991, Ruth F. Wolfe included it as a member of the proposed Tiflis asteroid family. This is classed as an S-type asteroid in the Tholen taxonomy. It spans a girth of approximately 23.6 km and rotates on its axis every 9.85 hours. References External links Discovery Circumstances: Numbered Minor Planets Background asteroids Tiflis Tiflis S-type asteroids (Tholen) L-type asteroids (SMASS) 19130430

3033421

https://en.wikipedia.org/wiki/760%20Massinga

760 Massinga

760 Massinga (prov. designation: or ) is a large background asteroid from the outer regions of the asteroid belt, approximately in diameter. It was discovered by German astronomer Franz Kaiser at the Heidelberg Observatory on 28 August 1913. The stony S-type asteroid has a rotation period of 10.7 hours and is somewhat elongated in shape. It was named in memory of Adam Massinger (1888–1914), a German astronomer at Heidelberg who was killed in World War I. Orbit and classification Massinga 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 2.4–3.9 AU once every 5 years and 7 months (2,039 days; semi-major axis of 3.15 AU). Its orbit has an eccentricity of 0.23 and an inclination of 13° with respect to the ecliptic. Discovery Massinga was discovered by Franz Kaiser at the Heidelberg-Königstuhl State Observatory in southwest Germany on 28 August 1913. On the same night, it was independently discovered by Russian astronomer Grigory Neujmin at the Simeiz Observatory on the Crimean peninsula. The Minor Planet Center, however, only credits Franz Kaiser with the discovery. The body's observation arc begins at Heidelberg on 8 November 1914, more than a year after its official discovery observation. Naming This minor planet was named after Adam Massinger (1888–1914), a German astronomer and discoverer of minor planets at Heidelberg who died in the First Battle of Ypres during World War I on 21 October 1914. An obituary was published by Max Wolf in the astronomical journal Astronomische Nachrichten. The was mentioned in The Names of the Minor Planets by Paul Herget in 1955 (). Physical characteristics In the Tholen classification, Massinga is a common, stony S-type asteroid, though with an unusual spectrum (SU), while in the Tholen- and SMASS-like taxonomic variants of the Small Solar System Objects Spectroscopic Survey (S3OS2), it is an S-type and SL-type, latter which transitions to the uncommon L-type, respectively. Rotation period In December 1999, a rotational lightcurve of Massinga was obtained from photometric observations by Robert A. Koff at his observatory in Colorado. Lightcurve analysis gave a rotation period of hours with a brightness variation of magnitude (). In March 2006, Laurent Bernasconi and Rui Goncalves determined a similar 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, the Japanese Akari satellite, and the Infrared Astronomical Satellite IRAS, Massinga measures (), () and () kilometers in diameter and its surface has an albedo of (), () and (), respectively. The Collaborative Asteroid Lightcurve Link derives an albedo of 0.2392 and a diameter of 71.47 kilometers based on an absolute magnitude of 7.9. On 29 February 2012, an asteroid occultation of Massinga gave a best-fit ellipse dimension of (), with a high quality rating of 3. 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 000760 Discoveries by Franz Kaiser Named minor planets 000760 19130828

3033424

https://en.wikipedia.org/wiki/761%20Brendelia

761 Brendelia

761 Brendelia is a minor planet orbiting the Sun that was discovered by German astronomer Franz Kaiser on September 8, 1913, and named after Otto Rudolf Martin Brendel. It is orbiting at a distance of from the Sun with a period of and an orbital eccentricity of 0.065297. The orbital plane is inclined at an angle of 2.16° to the plane of the ecliptic. This is a member of the dynamic Koronis family of asteroids that most likely formed as the result of a collisional breakup of a parent body. It is an SC-type asteroid that is spinning with a period of . References External links Koronis asteroids Brendelia Brendelia SC-type asteroids (Tholen) 19130908

3033441

https://en.wikipedia.org/wiki/763%20Cupido

763 Cupido

763 Cupido (prov. designation: or ) is a Flora asteroid, tumbler and slow rotator from the inner regions of the asteroid belt, approximately in diameter. It was discovered on 25 September 1913, by German astronomer Franz Kaiser at the Heidelberg-Königstuhl State Observatory in southwest Germany. The S/L-type asteroid has an exceptionally long rotation period of 151 hours. It was named by its Latin name after Cupid, the Roman god of erotic love, attraction and affection. Orbit and classification When applying the synthetic hierarchical clustering method (HCM) by Nesvorný, or the 1995 HCM-analysis by Zappalà, Cupido 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. Cupido orbits the Sun in the inner asteroid belt at a distance of 1.9–2.6 AU once every 3 years and 4 months (1,226 days; semi-major axis of 2.24 AU). Its orbit has an eccentricity of 0.17 and an inclination of 4° with respect to the ecliptic. The body's observation arc begins at Yerkes Observatory in September 1933, or 20 years after to its official discovery observation by Franz Kaiser at Heidelberg Observatory in 1913. Naming This minor planet was named "Cupido", the Latin name of Cupid, god of erotic love, attraction and affection in Roman mythology whose Greek counterpart is Eros (also see asteroid 433 Eros). Cupido was named due to its relative proximity to the Sun probably by Swedish astronomer Bror Ansgar Asplind (1890–1954) who was honored by asteroid 958 Asplinda. The was mentioned in The Names of the Minor Planets by Paul Herget in 1955 (). Physical characteristics In the SDSS-based taxonomy, Cupido is an SL-type that transitions from the common, stony S-type asteroids to the uncommon L-type asteroids. Rotation period In October 2017, a rotational lightcurve of Cupido was obtained from photometric observations by American astronomer Frederick Pilcher in collaboration with Vladimir Benishek at Belgrade Observatory and Daniel A. Klinglesmith at Etscorn Observatory . Lightcurve analysis gave a rotation period of hours with a brightness variation of magnitude (). The observations also showed that it is a tumbling asteroid, which wobbles on its non-principal axis rotation. During the same opposition, Tom Polakis at the Command Module Observatory also observed the asteroid and measured a period of hours and an amplitude of magnitude (). The results supersede a tentative period determination of hours by René Roy from 2005. Diameter and albedo According to the survey carried out by the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer (WISE), Cupido measures () kilometers in diameter and its surface has an albedo of (). Other publications by the WISE team give a mean-diameter of (), () and () with a corresponding albedo of (), () and (), respectively. The Collaborative Asteroid Lightcurve Link assumes a standard albedo for a Flora asteroid of 0.20 and calculates a diameter of 8.97 kilometers based on an absolute magnitude of 12.6. References External links Minor Planet Lightcurve Data, Frederick Pilcher 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 000763 Discoveries by Franz Kaiser Named minor planets 19130925

3033442

https://en.wikipedia.org/wiki/764%20Gedania

764 Gedania

764 Gedania (prov. designation: or ) is a large background asteroid from the outer regions of the asteroid belt, approximately in diameter. It was discovered on 26 September 1913, by German astronomer Franz Kaiser at the Heidelberg-Königstuhl State Observatory in southwest Germany. The carbonaceous C-type asteroid has a rotation period of 24.98 hours. It was named after the Polish city of Gdańsk where the discoverer was an assistant at the observatory during the 1920s. Orbit and classification Gedania 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 (2,092 days; semi-major axis of 3.2 AU). Its orbit has an eccentricity of 0.09 and an inclination of 10° with respect to the ecliptic. The body's observation arc begins with its first observation as at Heidelberg Observatory in November 1902, almost 11 years prior to its official discovery observation by Franz Kaiser. Naming This minor planet was named after the Latin name of the city of Gdańsk, Poland (formerly Free City of Danzig) where the discoverer, Franz Kaiser (1891–1962), was an assistant at the observatory during the early 1920s. The official naming citation was mentioned in The Names of the Minor Planets by Paul Herget in 1955 (). Asteroid 1419 Danzig was also named by its German name for the city of Gdańsk. Physical characteristics In the Tholen classification, Gedania is a common carbonaceous C-type asteroid. It has also been classified as an hydrated Ch-type and as a Caa type in the Tholen- and SMASS-like taxonomic variant of the Small Solar System Objects Spectroscopic Survey (S3OS2). Rotation period In February 2006, a rotational lightcurve of Gedania was obtained from photometric observations by collaborating astronomers Roberto Crippa, Federico Manzini , René Roy, Donn Starkey, Raoul Behrend and Laurent Bernasconi. Lightcurve analysis gave a rotation period of hours with a brightness variation of magnitude (). Observations by Aznar, Brinsfield and Pál, gave an alternative period determination of , and hours, respectively (). 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 and the Japanese Akari satellite, Gedania measures , and kilometers in diameter and its surface has an albedo of , and , respectively. The Collaborative Asteroid Lightcurve Link derives an albedo of 0.0754 and a diameter of 58.18 kilometers based on an absolute magnitude of 9.6. An alternative mean-diameter measurement published by the WISE team gave () with corresponding albedo of (). On 5 February 2006, an asteroid occultation of Gedania gave a best-fit ellipse dimension of (), with a poor quality rating of 1. 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 000764 Discoveries by Franz Kaiser Named minor planets 000764 19130926

3033443

https://en.wikipedia.org/wiki/765%20Mattiaca

765 Mattiaca

765 Mattiaca is a minor planet, specifically an asteroid orbiting in the asteroid belt. Photometric observations made in 2011–2012 at the Organ Mesa Observatory in Las Cruces, New Mexico produced an irregular light curve and a period of 3.4640 ± 0.0001 hours with a brightness variation of 0.09 ± 0.01 in magnitude. Mattiacum was the Latin name for the city of Wiesbaden, Germany, birthplace of the discoverer. References External links Background asteroids Mattiaca 19130926 Mattiaca

3033444

https://en.wikipedia.org/wiki/766%20Moguntia

766 Moguntia

766 Moguntia is a minor planet orbiting the Sun. It was discovered on 29 September 1913 at Heidelberg by German astronomer Franz Kaiser, and is named after Mainz, ancient Moguntiacum. This object is a member of the same dynamic asteroid group as 221 Eos, the Eos family. It is orbiting at a distance of from the Sun with a period of and an eccentricity (ovalness) of 0.097. The orbital plane is inclined at an angle of 10.1° to the plane of the ecliptic. This is an M-type asteroid with a near infrared spectrum that is similar to CO/CV meteorites. An absorption feature at around 1 μm suggests the presence of olivine on the surface. 766 Moguntia spans approximately 31.2 km in girth and is spinning with a rotation period of 4.82 hours. References External links Lightcurve plot of 766 Moguntia, Palmer Divide Observatory, B. D. Warner (2010) 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 Eos asteroids Moguntia Moguntia MU-type asteroids (Tholen) 19130929

3033447

https://en.wikipedia.org/wiki/767%20Bondia

767 Bondia

767 Bondia (prov. designation: or ) is a Themis asteroid from the outer regions of the asteroid belt, approximately in diameter. It was discovered on 23 September 1913, by American astronomer Joel Hastings Metcalf at his observatory in Winchester, Massachusetts. The B-type asteroid has a rotation period of 8.3 hours. It was named after William Cranch Bond (1789–1859) and his son George Phillips Bond (1825–1865), both American astronomers and directors of the Harvard College Observatory in Cambridge, Massachusetts. Orbit and classification Bondia is a core member 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 2.6–3.7 AU once every 5 years and 6 months (2,015 days; semi-major axis of 3.12 AU). Its orbit has an eccentricity of 0.18 and an inclination of 2° with respect to the ecliptic. The Themistian asteroid was first observed as () at Heidelberg Observatory on 26 September 1902. The body's observation arc begins at Bergedorf Observatory in September 1915, or two years after its official discovery observation by Metcalf at Winchester Observatory. Naming This minor planet was named after American astronomers William Cranch Bond (1789–1859) and his son George Phillips Bond (1825–1865), both directors of the Harvard College Observatory in Cambridge, Massachusetts. Former co-discovered and pioneered the use of photographic plates in astronomy. The latter is best known for his 1848 co-discovery of Hyperion, a moon of Saturn. He also discovered Saturn's faint C Ring, also known as Crepe Ring. The was mentioned in The Names of the Minor Planets by Paul Herget in 1955 (). The lunar craters W. Bond and G. Bond were named in honor of the two American astronomers. In addition, Martian crater Bond was named after George Phillips. Physical characteristics In the Bus–Binzel SMASS classification, Bondia is a B-type asteroid, a brighter variant of the common carbonaceous C-type asteroid. Rotation period In October 2018, a rotational lightcurve of Bondia was obtained from photometric observations by Mexican astronomers at the National Astronomical Observatory in San Pedro Mártir (OAN-SPM). Lightcurve analysis gave a well defined rotation period of hours with a brightness variation of magnitude () and supersedes a previous observation by Szabó from 2016, who determined a period of at least hours and a low amplitude (). 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), Bondia measures and kilometers in diameter and its surface has an albedo between and , respectively. The Collaborative Asteroid Lightcurve Link derives an albedo of 0.0857 and a diameter of 41.40 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 (). 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 000767 Discoveries by Joel Hastings Metcalf Named minor planets 000767 19130923

3033450

https://en.wikipedia.org/wiki/768%20Struveana

768 Struveana

768 Struveana is a minor planet orbiting the Sun. The asteroid was named jointly in honor of Baltic German astronomers Friedrich Georg Wilhelm von Struve, Otto Wilhelm von Struve and Karl Hermann Struve. References External links Discovery Circumstances: Numbered Minor Planets Meliboea asteroids Struveana Struveana X-type asteroids (Tholen) 19131004 Struve family

3033459

https://en.wikipedia.org/wiki/769%20Tatjana

769 Tatjana

769 Tatjana is a minor planet orbiting the Sun. The body was named such after Tatiana Larina, protagonist of Alexander Pushkin's poem "Eugene Onegin". It's possible that the name was suggested by the provisional designation of the asteroid, 1913 TA, but unlike bodies named by Wolf, Knopff and Metcalf in the years 1905–1909, there's no naming pattern to support this. References External links Discovery Circumstances: Numbered Minor Planets 000769 Discoveries by Grigory Neujmin Named minor planets 19131006

3033463

https://en.wikipedia.org/wiki/771%20Libera

771 Libera

771 Libera, provisional designation 1913 TO, is a metallic asteroid from the middle region of the asteroid belt, about 29 kilometers in diameter. It was discovered by Austrian astronomer Joseph Rheden at the Vienna Observatory in Austria, on 21 November 1913. Description The metallic X-type asteroid orbits the Sun at a distance of 2.0–3.3 AU once every 4 years and 4 months (1,576 days). Its orbit shows an eccentricity of 0.25 and is tilted by 15 degrees to the plane of the ecliptic. A photometric observation of the asteroid's light-curve performed at the Palmer Divide Observatory during 1999 rendered a rotation period of hours with a brightness variation of 0.57 magnitude. The result concurs with several previous observations, including a photometric analysis conducted over a twelve-year interval. According to the surveys carried out by the Infrared Astronomical Satellite, IRAS, the Japanese Akari satellite, and the U.S. Wide-field Infrared Survey Explorer with its subsequent NEOWISE mission, the asteroid's surface has an albedo of 0.13 and 0.14, respectively, while the Collaborative Asteroid Lightcurve Link publishes a slightly lower figure of 0.12 from an alternative result of the Supplemental IRAS Minor Planet Survey. The minor planet was named by Mrs. Hedwig Rheden in honor of a friend of the discoverer. References External links Lightcurve plot of 771 Libera, 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 000771 Discoveries by Joseph Rheden Named minor planets 000771 000771 19131121

3033464

https://en.wikipedia.org/wiki/772%20Tanete

772 Tanete

772 Tanete is an asteroid from the asteroid belt. Since 2004 it has been observed in stellar occultation four times. Its size is best described by an ellipsoid measuring x . Analysis of a light curve captured during 2014 shows a synodic rotation period of with an amplitude of 0.15 magnitude. In 1984, a fly-by of 772 Tanete was considered for a Mariner Mark II rendezvous mission with the short period comet 22P/Kopff. See also List of Solar System objects by size References External links 000772 Discoveries by Adam Massinger Named minor planets 000772 19131219

3033466

https://en.wikipedia.org/wiki/770%20Bali

770 Bali

770 Bali is a minor planet orbiting the Sun. It is a member of the Flora family. It was discovered on 31 October 1913, by German astronomer Adam Massinger at the Heidelberg Observatory in southwest Germany. The asteroid was probably named after the Indonesian island of Bali, as the discoverer had named a couple other asteroids after places in Indonesia. The alternative hypothesis is that it was named after Bali, king of the Daityas in Hindu mythology. References External links 000770 Discoveries by Adam Massinger Named minor planets 000770 19131031

3033468

https://en.wikipedia.org/wiki/773%20Irmintraud

773 Irmintraud

773 Irmintraud, provisional designation 1913 TV, is a dark and reddish, rare-type asteroid from the outer region of the asteroid belt, about 92 kilometers in diameter. It was discovered on 22 December 1913, by German astronomer Franz Kaiser at Heidelberg Observatory in southern Germany. The asteroid is classified as a D-type and T-type body in the Tholen and SMASS taxonomy, respectively. The rare spectral T-type is similar to D-types which are often found among Jupiter trojans thought to have originated from the Kuiper belt. It orbits the Sun at a distance of 2.6–3.1 AU once every 4 years and 10 months (1,763 days). Its orbit is tilted by 17 degrees to the plane of the ecliptic and shows a low eccentricity of 0.08. According to the surveys carried out by the Infrared Astronomical Satellite, IRAS, the Japanese Akari satellite, and the Wide-field Infrared Survey Explorer with its subsequent NEOWISE mission, the minor planet's low albedo lies in the range of 0.04–0.05. It has a well-defined rotation period of 6.75 hours, determined by several concurring observations. 773 Irmintraud commemorates the antiquated German feminine name, Irmtraud, that appears frequently in old songs and sagas. The asteroid is a likely source of the Tagish Lake meteorite which landed in Canada on January 18, 2000. History In 1992, Larry Lebofsky and colleagues published an article in which they noted that "unaltered asteroids are thought to represent the raw materials available for terrestrial planet formation and so are important to our understanding of the origin and evolution of the Solar System." Since at least 1980, it was believed that D-type asteroids were unaltered asteroids, ultraprimitive in composition and composed largely of hydrated silicates and organic material. However, in analyzing the spectra of 773 Irmintraud for the water of hydration band (the 3-μm absorption feature of hydrated silicates), Lebofsky discovered the first D-type asteroid to show the water of hydration band on the surface of the asteroid. Lebofsky concluded that 773 Irmintraud had undergone an alteration process typically seen in a C-type asteroid, making 773 Irmintraud and perhaps other D-type asteroids less likely to represent the raw materials available for terrestrial planet formation. In addition, the discovery of water of hydration band on 773 Irmintraud meant that there may be major differences in mineralogy within individual type classification and astronomers must be careful in assuming that the C-, D-, and other type classification relate directly to mineralogy. In 1997, NASA added 773 Irmintraud and eventually over one million other names to a microchip placed on board the Stardust spacecraft that launched February 7, 1999. Placing the names onto the Stardust spacecraft was a public outreach effort. In particular, this served to promote public interest, awareness and support of the space program. In September 2001, there was speculation that Tagish Lake meteorite which struck in British Columbia, Canada on January 18, 2000, was derived from a D-type asteroid, since the spectral shape and brightness of the meteorite was similar to D-type asteroids. Of the three studied, the 0.032 IRAS albedos (8) of 368 Haidea and the 0.033 IRAS albedos (8) of 773 Irmintraud are both considered close to the reflectance of the Tagish Lake meteorite. Moreover, even though 368 Haidea was closest spectrally to the Tagish Lake meteorite, 773 Irmintraud was no more than 0.034 AU to a chaotic zone associated with one of the Kirkwood gaps due to the mean motion resonance with Jupiter. This made 773 Irmintraud the closest of the three candidates to the associated chaotic zone and thus the most likely of the three as the source of the 2000 Earth impacted meteorite. The idea that humans held a piece of the asteroid 773 Irmintraud spurred others to act. In 2002, the University of Tokyo performed near-infrared photometric and spectroscopic observations of 773. In addition, the University obtained an accurate lightcurve in Japan through visible photometry and ultimately found a gap between K- and L-band spectra. From this, the university concluded that results support the idea that Tagish Lake meteorite has a link with D-type asteroids. On May 22, 2007, at 06:07 UT, Irmintraud occulted TYC 4908-00263-1, a 10.7 magnitude star in the constellation Sextans, for observers along a path across New Zealand. References External links NASA Target Catalog Information () Lightcurve plot of 773 Irmintraud, 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 000773 Discoveries by Franz Kaiser Named minor planets Natural history of British Columbia Natural history of Yukon 000773 000773 19131222

3033471

https://en.wikipedia.org/wiki/775%20Lumi%C3%A8re

775 Lumière

775 Lumière is a minor planet orbiting the Sun. The apparent magnitude is 10.40. The diameter is 33.58 kilometers. Its rotational period is 6.103 hours, and the albedo is .108. The name honors Auguste and Louis Lumiere and the company making photographic film for astronomers in France. References External links Eos asteroids Lumiere Lumiere Auguste and Louis Lumière S-type asteroids (Tholen) 19140106

3033472

https://en.wikipedia.org/wiki/774%20Armor

774 Armor

774 Armor is a minor planet (specifically an asteroid) orbiting in the main belt. It was discovered on December 13, 1913, in Paris by French astronomer Charles le Morvan and was named after the Celtic region of Armorica. The asteroid is orbiting at a distance of with a period of and an eccentricity of 0.169. The orbital plane is inclined by an angle of 5.56° to the plane of the ecliptic. In the SMASS-I taxonomy, this is classified as an S-type asteroid. It spans a girth of approximately 50 km. The rotation of this asteroid is commensurate with the length of an Earth day, requiring measurements from more than one latitude for full coverage. Photometric observations from the US and Australia in 2012 provided an estimated rotation period of with a brightness variation of in magnitude. This is consistent with the results of an earlier study in 2006. References External links Lightcurve plot of 774 Armor, 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 S-type asteroids (SMASS) 000774 Discoveries by C. le Morvan Named minor planets 19131219 Armorica

3033473

https://en.wikipedia.org/wiki/776%20Berbericia

776 Berbericia

776 Berbericia is a minor planet orbiting the Sun. A main-belt C-type asteroid, it was discovered on 24 January 1914 by astronomer Adam Massinger at Heidelberg Observatory in southwest Germany. It was named by Max Wolf in honor of Adolf Berberich (1861–1920), a German astronomer. The spectra of the asteroid displays evidence of aqueous alteration. Description In the late 1990s, a network of astronomers worldwide gathered lightcurve data that was ultimately used to derive the spin states and shape models of 10 new asteroids, including (776) Berbericia. The computed shape model for this asteroid is described as "asymmetric with sharp edges". Richard P. Binzel and Schelte Bus further added to the knowledge about this asteroid in a lightwave survey published in 2003. This project was known as Small Main-belt Asteroid Spectroscopic Survey, Phase II or SMASSII, which built on a previous survey of the main-belt asteroids. The visible-wavelength (0.435-0.925 micrometre) spectra data was gathered between August 1993 and March 1999. References External links 000776 Discoveries by Adam Massinger Named minor planets 000776 000776 19140124

3033474

https://en.wikipedia.org/wiki/777%20Gutemberga

777 Gutemberga

777 Gutemberga (prov. designation: or ) is a dark and large background asteroid, approximately in diameter, from the outer regions of the asteroid belt. It was discovered by German astronomer Franz Kaiser at the Heidelberg-Königstuhl State Observatory on 24 January 1914. The carbonaceous C-type asteroid (Cb) has a rotation period of 12.8 hours. It was named after Johannes Gutenberg (ca. 1400–1468), who introduced the printing press to Europe and started the Printing Revolution. Orbit and classification Gutemberga 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 2.9–3.6 AU once every 5 years and 10 months (2,119 days; semi-major axis of 3.23 AU). Its orbit has an eccentricity of 0.11 and an inclination of 13° with respect to the ecliptic. The body's observation arc begins at Heidelberg on 22 December 1924, almost 11 years after its official discovery observation. Naming This minor planet was named after Johannes Gutenberg (ca. 1400–1468), a German inventor who started the Printing Revolution with the introduction of mechanical movable type printing. Gutenberg lived and died in Mainz and the neighboring Eltville am Rhein. The was mentioned in The Names of the Minor Planets by Paul Herget in 1955 (). The crater Gutenberg on the Moon and the feature Rimae Gutenberg, a 223-kilometer long groove near the crater, were also named after him. Physical characteristics In the Tholen-like taxonomy of the Small Solar System Objects Spectroscopic Survey (S3OS2), Gutemberga is a common, carbonaceous C-type asteroid. In the Bus–Binzel SMASS-like taxonomic variant of the S3OS2, it is a Cb-subtype, which transitions from the C-type to the somewhat brighter B-type asteroid. Rotation period In January 218, a rotational lightcurve of Gutemberga 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 (). The result supersedes observations by Otmar Nickel of Astronomical Consortium of Mainz from February 2001, which gave a period of hours with an amplitude of magnitude (), and observations by Astronomers at the Palomar Transient Factory in California, with a period of hours and an amplitude of magnitude.(). 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, Gutemberga measures (), () and () kilometers in diameter and its surface has an albedo of (), () and (), respectively. The Collaborative Asteroid Lightcurve Link derives an albedo of 0.0494 and a diameter of 65.57 kilometers based on an absolute magnitude of 9.8. Alternative mean-diameter measurements published by the WISE team include () and () with corresponding albedos of () and (). On 27 June 2008, an asteroid occultation of Gutemberga gave a best-fit ellipse dimension of (), with a poor quality rating of 1. These timed observations are taken when the asteroid passes in front of a distant star. Notes References External links Wie schnell dreht sich Gutenberg im All? ( 777 Gutemberga), Otmar Nickel, Astronomical Consortium of Mainz (AAG Mainz) 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 000777 Discoveries by Franz Kaiser Named minor planets 19140124

3033479

https://en.wikipedia.org/wiki/778%20Theobalda

778 Theobalda

778 Theobalda is a minor planet orbiting the Sun, in the main asteroid belt. It was discovered by Franz Kaiser on 25 January 1914 and was named after his father, Theobald Kaiser. This is an F-type asteroid that spans ~64 km in girth. It rotates on its axis once every 11.7 hours. 778 Theobalda is orbiting from the Sun with an eccentricity (ovalness) of 0.25 and a period of . The orbital plane is inclined at an angle of 13.7° to the plane of the ecliptic. 778 Theobalda is the namesake and largest member of a family of 128 minor planets in the outer belt. The Theobalda asteroid family was likely formed  million years ago from a collision-shattered parent body that had a diameter of around . References External links Theobalda asteroids Theobalda Theobalda F-type asteroids (Tholen) 19140125

3033480

https://en.wikipedia.org/wiki/779%20Nina

779 Nina

779 Nina (prov. designation: or ) is a large background asteroid, approximately in diameter, located in the central region of the asteroid belt. It was discovered on 25 January 1914, by Russian astronomer Grigory Neujmin(1886-1946) at the Simeiz Observatory on the Crimean peninsula. The metallic X-type asteroid with an intermediate albedo has a rotation period of 11.2 hours. It was named after the discoverer's sister, Nina Neujmina (Tsentilovich) (1889–1971). Orbit and classification Nina 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 main-belt at a distance of 2.1–3.3 AU once every 4 years and 4 months (1,588 days; semi-major axis of 2.66 AU). Its orbit has an eccentricity of 0.23 and an inclination of 15° with respect to the ecliptic. The body's was first observed as and at Heidelberg Observatory on 16 December 1908 and 14 October 1912, respectively. The observation arc begins at Vienna Observatory on 31 July 1916, more than two years after to its official discovery observation at Simeiz Observatory on Crimea. Naming This minor planet was after Nina Nikolaevna Neujmina (Tsentilovich) (1889–1971), mathematician and sister of Russian discoverer Grigory Neujmin(1886-1946). Physical characteristics In the Bus–Binzel SMASS classification, Nina is an X-type asteroid. It is also an X-type in both the Tholen- and SMASS-like taxonomy of the Small Solar System Objects Spectroscopic Survey (S3OS2). Belskaya classifies Nina as a metallic M-type asteroid, which is the equivalent spectral type in the Tholen taxonomy for X-types with an intermediate albedo (see below). Rotation period In June 1981, a rotational lightcurve of Nina was obtained from photometric observations by Alan Harris at the Table Mountain and Lowell observatories. Lightcurve analysis gave a rotation period of hours with a brightness variation of magnitude (). It was confirmed by Brian Warner at his Palmer Divide Observatory in Colorado in January 2009, who determined a period of hours with an amplitude of magnitude (). In September 2012, French amateur astronomer Gérald Rousseau obtained a period of hours with an amplitude of magnitude (). 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, Nina measures (), () and () kilometers in diameter and its surface has an albedo of (), () and (), respectively. The Collaborative Asteroid Lightcurve Link adopts Petr Pravec's revised WISE-albedo of 0.1694 and takes a diameter of 77.46 kilometers based on an absolute magnitude of 8.1. The WISE team also published an alternative mean-diameter of () with an albedo of (). On 10 November 2005, an asteroid occultation of Nina gave a best-fit ellipse dimension of (), with a quality rating of 2. 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 000779 Discoveries by Grigory Neujmin Named minor planets 000779 19140125

3033482

https://en.wikipedia.org/wiki/780%20Armenia

780 Armenia

780 Armenia is a minor planet in the asteroid belt orbiting the Sun. It is named after the Kingdom of Armenia, now Armenia. This object is orbiting at a distance of with an eccentricity of 0.097 and a period of . The orbital plane is inclined at an angle of 19.1° to the plane of rotation. This asteroid spans a girth of ~94 km. The long rotation period of this asteroid necessitated light curve data from more than one latitude. The overlapping data provided a solution with a period of and a brightness amplitude of in magnitude. This object is the namesake of the Armenia family, a family of 13–76 asteroids that share similar spectral properties and orbital elements; hence they may have arisen from the same collisional event. All members have a relatively high orbital inclination. References External links Discovery Circumstances: Numbered Minor Planets 000780 Discoveries by Grigory Neujmin Named minor planets 19140125

3033492

https://en.wikipedia.org/wiki/781%20Kartvelia

781 Kartvelia

781 Kartvelia is a minor planet orbiting the Sun that was discovered by Russian astronomer Grigory Neujmin on January 25, 1914. Kartvelia comes from the historic name for the inhabitants of the nation of Georgia. This object is orbiting at a distance of with an eccentricity (ovalness) of 0.12 and a period of . The orbital plane is inclined at an angle of 19.1° to the plane of the ecliptic. This asteroid is rotating with a period of 19.0 hours and spans an estimated girth of 66 km. It is tentatively classified as type CPU in the Tholen taxonomic system, with the C indicating a carbonaceous object. This is the namesake of a family of 49–232 asteroids that share similar spectral properties and orbital elements; hence they may have arisen from the same collisional event. All members have a relatively high orbital inclination. References External links Discovery Circumstances: Numbered Minor Planets 000781 Discoveries by Grigory Neujmin Named minor planets 000781 000781 19140125

3033494

https://en.wikipedia.org/wiki/782%20Montefiore

782 Montefiore

782 Montefiore is a minor planet, specifically an asteroid orbiting in the asteroid belt that was discovered by Austrian astronomer Johann Palisa on 18 March 1914 and named for Clarice Sebag-Montefiore, wife of Alfons von Rothschild of Vienna. It is orbiting from the Sun with an eccentricity of 0.04 and a period of . The orbital plane of this asteroid is inclined by an angle of 5.26° to the plane of the ecliptic. 10μ radiometric data collected from Kitt Peak in 1975 gave a diameter estimate of 15 km. Photometric light curve studies from 1997 onward give a consistent rotation period of 4.07 hours. References External links 000782 Discoveries by Johann Palisa Named minor planets 000782 000782 19140318

3033495

https://en.wikipedia.org/wiki/783%20Nora

783 Nora

783 Nora (prov. designation: or ) is a dark background asteroid from the inner regions of the asteroid belt. It was discovered by Austrian astronomer Johann Palisa at the Vienna Observatory on 18 March 1914. The carbonaceous C-type asteroid has a longer-than average rotation period of 55.5 hours and measures approximately in diameter. It was likely named after Nora Helmer, principal character in the play A Doll's House by Norwegian poet Henrik Ibsen. Orbit and classification Nora 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 1.8–2.9 AU once every 3 years and 7 months (1,310 days; semi-major axis of 2.34 AU). Its orbit has an eccentricity of 0.23 and an inclination of 9° with respect to the ecliptic. The body's observation arc begins with its first observation as at Heidelberg Observatory on 28 August 1911, more than two years prior to its official discovery observation at Vienna Observatory. Naming This minor planet was likely named after Nora Helmer, the heroine in the play A Doll's House (1879) by Norwegian poet Henrik Ibsen (1828–1906). The name was given by the discoverer's friends. The was also mentioned in The Names of the Minor Planets by Paul Herget in 1955 (). Physical characteristics In the Bus–Binzel SMASS classification, Nora is a common, carbonaceous C-type asteroid. In the Tholen classification it is one of few asteroids considered unclassifiable. Rotation period In March 2018, a rotational lightcurve of Nora 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 previous observations by European astronomers at the La Silla, Haute Provence and Hoher List observatories during the 1990s which gave two periods of and with an amplitude of and magnitude, respectively (). In April 2007, French astronomer Arnaud Leroy determined a period of and a brightness variation of 0.01 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, Nora measures (), () and () kilometers in diameter and its surface has an albedo of (), () and (), respectively. The Collaborative Asteroid Lightcurve Link derives an albedo of 0.0404 and a diameter of 39.84 kilometers based on an absolute magnitude of 11.1. Alternative mean-diameter measurements published by the WISE team include (), (), (), () and () with corresponding albedos of (), (), (), () and (). On 4 May 2004, an asteroid occultation of Nora gave a best-fit ellipse dimension of (), with a poor quality rating of 1. 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 000783 Discoveries by Johann Palisa Named minor planets 000783 000783 19140318

3033496

https://en.wikipedia.org/wiki/784%20Pickeringia

784 Pickeringia

784 Pickeringia (prov. designation: or ) is a large background asteroid, approximately in diameter, located in the outer region of the asteroid belt. It was discovered on 20 March 1914, by American astronomer Joel Hastings Metcalf at the Winchester Observatory in Massachusetts. The dark C-type asteroid has a rotation period of 13.1 hours and an irregular shape. It was named after American astronomers Edward Charles Pickering (1846–1919) and his brother William Henry Pickering (1858–1938). Orbit and classification Pickeringia 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 2.3–3.8 AU once every 5 years and 5 months (1,989 days; semi-major axis of 3.1 AU). Its orbit has an eccentricity of 0.24 and an inclination of 12° with respect to the ecliptic. The body's observation arc begins at Heidelberg Observatory on 30 September 1921, more than seven years after its official discovery observation at Winchester Observatory . Naming This minor planet was named after American astronomers Edward Charles Pickering (1846–1919) and his brother William Henry Pickering (1858–1938), who were the directors of the Harvard Observatory and the Boyden Station at Arequipa, respectively. William Henry also discovered Phoebe, an irregular moon of Saturn. The was mentioned in The Names of the Minor Planets by Paul Herget in 1955 (). The lunar crater Pickering and the Martian crater Pickering were also named in honor of the two astronomers. Physical characteristics In the Bus–Binzel SMASS classification, Pickeringia is a common, carbonaceous C-type asteroid. Rotation period In January 2017, a rotational lightcurve of Pickeringia was obtained from photometric observations by the Spanish group of asteroids observers (OBAS). Lightcurve analysis gave a rotation period of hours with a brightness variation of magnitude (). The result supersedes observations taken during the 1990s by European astronomers using the ESO 0.5-metre telescope at La Silla Observatory, Chile, which gave a period of hours with an amplitude of magnitude (). as well as a period determination by French amateur astronomer Laurent Bernasconi in December 2004, which gave and an amplitude of magnitude (). Modeled lightcurve Two modeled lightcurves, published by Josef Ďurech and Josef Hanuš in 2016, using photometric data from the Lowell Photometric Database (LPD) and other sources, gave a sidereal period of and , respectively. Each modeled lightcurve also determined two spin axes of (99.0°, 67.0°) and (283.0°, 30.0°), as well as (282.0°, 35.0°) and (103.0°, 68.0°) in ecliptic coordinates (λ, β), respectively. The online version of the Database of Asteroid Models from Inversion Techniques gives two poles at (103°, 68.0°) and (282°, 35.0°) with a nearly identical sidereal period. 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, Pickeringia measures (), () and () kilometers in diameter and its surface has an albedo of (), () and (), respectively. The Collaborative Asteroid Lightcurve Link derives an albedo of 0.0423 and a diameter of 89.19 kilometers based on an absolute magnitude of 9.3. while Carry gives a diameter of and estimates a mass of kilogram from an unrealistic density of . Alternative mean-diameter measurements published by the WISE team include (), () and () with corresponding albedos of (), () and (). On 7 August 2008, an asteroid occultation of Pickeringia gave a best-fit ellipse dimension of (), with a poor quality rating of 1. 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 000784 Discoveries by Joel Hastings Metcalf Named minor planets 000784 19140320

3033497

https://en.wikipedia.org/wiki/785%20Zwetana

785 Zwetana

785 Zwetana is a minor planet orbiting the Sun that was discovered by Adam Massinger, an assistant at the Heidelberg Observatory, on March 30, 1914. It was named for the daughter of Kiril Popoff, a Bulgarian astronomer. This asteroid is orbiting from the Sun with an eccentricity (ovalness) of 0.21 and a period of . The orbital plane is inclined by an angle of 12.8° to the plane of the ecliptic. This asteroid spans a girth of and it has a Tholen taxonomic class of M. Radar observations indicate that it is almost certainly metallic. The near infrared spectra suggests the presence of spinel on the surface, which is indicative of calcium–aluminium-rich inclusions. The best meteorite analog to the near infrared spectrum of this object is the enstatite chondrite, Abee. In 1990, the asteroid was observed from the European Southern Observatory, allowing a composite light curve to be produced that showed a rotation period of and a brightness variation of in magnitude. 2013 observations from the Palmer Divide Observatory found a rotation period of 8.885 hours with a magnitude amplitude of 0.18. This is consistent with other published results. References External links 000785 Discoveries by Adam Massinger Named minor planets 000785 000785 19140330

3033502

https://en.wikipedia.org/wiki/786%20Bredichina

786 Bredichina

786 Bredichina (prov. designation: or ) is a carbonaceous and very large background asteroid, approximately in diameter, located in the outer region of the asteroid belt. It was discovered by German astronomer Franz Kaiser at the Heidelberg-Königstuhl State Observatory on 20 April 1914. The elongated C-type asteroid has a longer than average rotation period of 29.4 hours. It was named after Russian astronomer Fyodor Bredikhin (1831–1904). Orbit and classification Bredichina 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 2.7–3.7 AU once every 5 years and 8 months (2,068 days; semi-major axis of 3.18 AU). Its orbit has an eccentricity of 0.16 and an inclination of 15° with respect to the ecliptic. The body's observation arc begins at Heidelberg Observatory on 21 April 1914, the night after its official discovery observation. Naming This minor planet was named after Fyodor Bredikhin (1831–1904), also known as Theodor or Feodor Alexandrovich Bredichin, a Russian astronomer and director of the Pulkovo Observatory. He has made important contributions to the study of comets. The was also mentioned in The Names of the Minor Planets by Paul Herget in 1955 (). The lunar crater Bredikhin is also named after him. Physical characteristics In the Tholen classification, Bredichina is a common, carbonaceous C-type asteroid. It is also a C-type and C0-type in the Tedesco and Barucci classification from the 1908s. Rotation period In March 2015, a rotational lightcurve of Bredichina was obtained from photometric observations by Spanish astronomers Alfonso Carreño , Amadeo Aznar , Enrique Arce , Pedro Brines , and Juan Lozano . Lightcurve analysis gave a rotation period of hours with a brightness variation of magnitude (). Previously, in August 2008, Argentine astronomer Ricardo Gil-Hutton derived period of hours with an amplitude of magnitude (). Tentative measurements were also made by Italian Nicola Cornero and Federico Manzini at the Sozzago Astronomical Station in May 2010, which gave a period of hours with an amplitude of magnitude (). The same period was also determined by Eric Barbotin in February 2020, though with a higher brightness variation of . 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, Bredichina 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 0.0730 and a diameter of 91.60 kilometers based on an absolute magnitude of 8.65, while Carry give a diameter of and estimates a mass of kilogramm. Alternative mean-diameter measurements published by the WISE team include (), (), (), () and () with corresponding albedos of (), (), (), () and (). On 10 January 2015, an asteroid occultation of Bredichina gave a best-fit ellipse dimension of (), indicative of a highly elongated shape, with a good quality rating of 3. 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 000786 Discoveries by Franz Kaiser Named minor planets 000786 19140420

3033505

https://en.wikipedia.org/wiki/787%20Moskva

787 Moskva

787 Moskva is a minor planet orbiting the Sun. It is a dynamic member of the Maria asteroid family orbiting near the 3:1 Kirkwood gap. This is an S-type (stony) asteroid spanning 27 km. The surface mineralogy is consistent with mesosiderite silicates. Object 1914 UQ, discovered 20 April 1914 by Grigory Neujmin, was named 787 Moskva, after the capital of Russia, Moscow (and retains that name to this day). Object 1934 FD discovered on 19 March 1934 by C. Jackson was given the sequence number 1317. In 1938, G. N. Neujmin found that asteroid 1317 and 787 Moskva were, in fact, the same object. Sequence number 1317 was later reused for the object 1935 RC discovered on 1 September 1935 by Karl Reinmuth; that object is now known as 1317 Silvretta. Photometric observations at the Palmer Divide Observatory in Colorado Springs, Colorado in 1999 were used to build a light curve for this object. The asteroid displayed a rotation period of 6.056 ± 0.001 hours and a brightness variation of 0.62 ± 0.01 in magnitude. References External links Lightcurve plot of 787 Moskva, 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 000787 Moskva Moskva 19140420

3033507

https://en.wikipedia.org/wiki/789%20Lena

789 Lena

789 Lena, provisional designation , is a metallic asteroid from the middle region of the asteroid belt, approximately 24 kilometers in diameter. It was discovered on 24 June 1914, by Soviet–Russian astronomer Grigory Neujmin at Simeiz Observatory on the Crimean peninsula, and named after the discoverer's mother. Orbit and classification Lena orbits the Sun in the middle main-belt at a distance of 2.3–3.1 AU once every 4 years and 5 months (1,608 days). Its orbit has an eccentricity of 0.15 and an inclination of 11° with respect to the ecliptic. Lenas observation arc begins with its first used observation made at Yerkes Observatory in 1935, or 21 years after its official discovery observation at Simeiz. Although its orbital elements resemble those of the asteroids in the Eunomia family, true members of this family have a S-type composition, so it is almost certainly an unrelated interloper. Physical characteristics In the SMASS taxonomy, Lena is an X-type asteroid. It has also been characterized as a metallic M-type asteroid by NASA's Wide-field Infrared Survey Explorer (WISE). Rotation period In 1993, a rotational lightcurve which was later proven incorrect, was obtained from photometric observations at the Félix Aguilar Observatory, Argentina. It gave an unusual lightcurve, indicating a very irregular shape and/or a relatively long rotation period of 22 hours with an exceptionally high amplitude of 1.5 in magnitude (). In August and September 2007, two reliable lightcurves were obtained by Italian astronomer Silvano Casulli and by members at the U.S.Oakley Observatory. Lightcurve analysis gave a period of and hours, with a brightness variation of 0.50 and of 0.40 magnitude, respectively (). Diameter and albedo According to the space-based surveys carried out by the Japanese Akari satellite and the NEOWISE mission of the WISE telescope, Lena measures between 20.6 and 23.9 kilometers in diameter, and its surface has an albedo of 0.137–0.186. The Collaborative Asteroid Lightcurve Link assumes a much lower albedo of 0.10 and calculates a diameter of 24.2 kilometer, as the lower the albedo (reflectivity), the larger a body's diameter, at a constant absolute magnitude (brightness). Naming This minor planet was named in honor of Elena ("Lena") Petrovna Neujmina (1860–1942), mother of the discovering astronomer Grigory Neujmin. Notes 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 000789 Discoveries by Grigory Neujmin Named minor planets 000789 19140624

3033510

https://en.wikipedia.org/wiki/788%20Hohensteina

788 Hohensteina

788 Hohensteina is a main-belt asteroid discovered on 4 April 1914 by Franz Kaiser at Heidelberg-Königstuhl State Observatory. Named for castle Hohenstein located in the Taunus mountains. References External links 000788 Discoveries by Franz Kaiser Named minor planets 19140428

3033511

https://en.wikipedia.org/wiki/790%20Pretoria

790 Pretoria

790 Pretoria is a minor planet orbiting the Sun that was discovered by English astronomer Harry Edwin Wood on January 16, 1912. It is a member of the Cybele group located beyond the core of the main belt (see Minor planet groups) and named after Pretoria, the capital city of South Africa. 10μ radiometric data collected from Kitt Peak in 1975 gave a diameter estimate of 175 km. In the present day it is estimated to be in diameter. Photometric measurements of the asteroid made in 2005 at the Palmer Divide Observatory showed a light curve with a period of 10.370 ± 0.002 hours and a brightness variation of 0.08 ± 0.03 in magnitude. Between 1998 and 2021, 790 Pretoria has been observed to occult twelve stars. References External links Lightcurve plot of 790 Pretoria, Palmer Divide Observatory, B. D. Warner (2009) 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 Cybele asteroids Pretoria Pretoria P-type asteroids (Tholen) 19120116

3033516

https://en.wikipedia.org/wiki/791%20Ani

791 Ani

791 Ani (prov. designation: or ) is a very large asteroid of the Meliboea family, located in the outer regions of the asteroid belt. It was discovered on 29 June 1914, by Russian astronomer Grigory Neujmin at the Simeiz Observatory on the Crimean peninsula. The dark carbonaceous C-type asteroid has a rotation period of 11.2 hours and measures approximately kilometers, with a mean-diameter of . It was named after the historic Armenian city of Ani. Orbit and classification When applying the hierarchical clustering method (HCM) to its proper orbital elements, Ani is a member of the Meliboea family (), a small family of carbonaceous asteroids in the outer main belt, named after its principal body, 137 Meliboea. However, according to another HCM-analysis by Milani and Knežević (AstDyS), it is a background asteroid as this analysis does not recognize the Meliboea family. Ani orbits the Sun in the outer asteroid belt at a distance of 2.5–3.7 AU once every 5 years and 6 months (2,015 days; semi-major axis of 3.12 AU). Its orbit has an eccentricity of 0.19 and an inclination of 16° with respect to the ecliptic. The body's observation arc begins at Algiers Observatory in North Africa on 6 December 1915, some 17 months after its official discovery observation at Simeiz Observatory. Naming This minor planet was named after the medieval city of Ani, which was destroyed by an earthquake in 1319. The ruins of the former capital of the Armenian kingdom are located near the border to Armenia, in what is now Turkey. Ani was known as "the city of 1001 churches". The was also mentioned in The Names of the Minor Planets by Paul Herget in 1955 (). Physical characteristics In the Tholen classification, Ani is a common, carbonaceous C-type asteroid. It is also a common C-type in the Tholen-like taxonomy of the Small Solar System Objects Spectroscopic Survey (S3OS2), while in the survey's SMASS-like taxonomic variant, the asteroid is a hydrated carbonaceous subtype (Ch). Rotation period and poles In May 2018, a rotational lightcurve of Ani was obtained from photometric observations by American amateur astronomer 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 (). In June 2002, Brian Warner at his Palmer Divide Observatory first observed this asteroid and later derived a period of hours and an amplitude of magnitude, based on poor data (). In December 2004, and in May 2007, two periods of and with a corresponding amplitude of and magnitude were determined by European astronomers Raymond Poncy as well as Yves Revaz, Raoul Behrend, Alain Klotz, Michel Hernandez, Robert Soubie, Jean-François Gauthier, Bernard Tregon, Pierre Antonini, Laurent Bernasconi, Federico Manzini , Yassine Damerdji and Horacio Correia. The two periods are slightly longer than twice Polakis period solution (). In April 2007, astronomers at the Oakley Observatory , Indiana, obtained a period of hours and an amplitude of magnitude (). In February 2011, French amateur astronomer René Roy determined a period of hours and a brightness variation of magnitude (). A modeled lightcurve by Josef Ďurech and Josef Hanuš, using photometric data including from the Lowell Photometric Database and from the Wide-field Infrared Survey Explorer (WISE) was published in 2018. It gave a sidereal period of and two spin axes at (94.0°, −25.0°) and (269.0°, 4.0°) 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, Ani 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 0.0329 and a diameter of 103.52 kilometers based on an absolute magnitude of 9.25. Alternative mean-diameter measurements published by the WISE team include (), (), () and () with corresponding albedos of (), (), () and (). On 7 April 2000, an asteroid occultation of Ani gave a best-fit ellipse dimension of () with a good quality rating of 3. 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 000791 Discoveries by Grigory Neujmin Named minor planets 000791 19140629

3033520

https://en.wikipedia.org/wiki/793%20Arizona

793 Arizona

793 Arizona is a minor planet orbiting the Sun that was discovered April 9, 1907 by American businessman Percival Lowell at Flagstaff. It was named for the state of Arizona. The object was independently discovered on April 17, 1907, by J. H. Metcalf at Taunton. This is a main belt asteroid orbiting from the Sun with a period of and an eccentricity (ovalness) of 0.13. The orbital plane is inclined at an angle of 15.8° to the plane of the ecliptic. Photometric observations at the Palmer Divide Observatory in Colorado Springs, Colorado during the winter of 2007–2008 were used to build a light curve for this asteroid. The asteroid displayed a period of and a brightness change of in magnitude. It spans a diameter of approximately 29 km and is a candidate D-type asteroid with an unusual spectrum. See also List of minor planets: 1–1000 References External links Lightcurve plot of 793 Arizona, Palmer Divide Observatory, B. D. Warner (2007) 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 000793 Discoveries by Percival Lowell 000793 Named minor planets 000793 000793 19070409

3033521

https://en.wikipedia.org/wiki/794%20Irenaea

794 Irenaea

794 Irenaea (prov. designation: or ) is a dark background asteroid from the outer regions of the asteroid belt. It was discovered on 27 August 1914, by Austrian astronomer Johann Palisa at the Vienna Observatory. The presumed C-type asteroid has a rotation period of 9.1 hours and measures approximately in diameter. It was likely named after Irene Hillebrand, daughter of Austrian astronomer Edmund Weiss (1837–1917). Orbit and classification Irenaea 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 2.2–4.1 AU once every 5 years and 6 months (2,021 days; semi-major axis of 3.13 AU). Its orbit has an eccentricity of 0.30 and an inclination of 5° with respect to the ecliptic. The body's observation arc begins at Bergedorf Observatory in Hamburg on 9 December 1915, more than a year after its official discovery observation at Vienna Observatory on 27 August 1914. Naming According to Alexander Schnell, this minor planet was likely named after Irene Hillebrand, née Weiss, daughter of Austrian astronomer Edmund Weiss (1837–1917), director of the Vienna Observatory, and wife to astronomer (1861–1939). The name received an aea-suffix as "Irene" was already given to asteroid 14 Irene. Palisa also named asteroid 722 Frieda after her daughter, Frieda Hillebrand. Physical characteristics Irenaea is an assumed, carbonaceous C-type asteroid. The asteroid's low albedo around 0.05 (see below) agrees with this assumption. Rotation period In May 2008, a rotational lightcurve of Irenaea was obtained from photometric observations by Italian amateur astronomer Silvano Casulli. Lightcurve analysis gave a rotation period of hours with a brightness variation of magnitude, indicative of an elongated shape (). 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, Irenaea 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 C-type asteroid of 0.057 and calculates a diameter of 30.59 kilometers based on an absolute magnitude of 11.3. 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 000794 Discoveries by Johann Palisa Named minor planets 19140827

3033523

https://en.wikipedia.org/wiki/792%20Metcalfia

792 Metcalfia

792 Metcalfia is a minor planet orbiting the Sun. It was discovered in 1907 by Joel Hastings Metcalf and was named after its discoverer. This is an X-type asteroid in the main belt some from the Sun. It has a rotation period of 9.17 hours and spans 61 km. The best fit meteorite analog is Gorlovka OC sample RS-CMP-048. See also List of minor planets: 1–1000 References External links 000792 Discoveries by Joel Hastings Metcalf Named minor planets 000792 19070320

3033525

https://en.wikipedia.org/wiki/795%20Fini

795 Fini

795 Fini (prov. designation: or ) is a dark and large background asteroid, approximately in diameter, located in the central region of the asteroid belt. It was discovered by Austrian astronomer Johann Palisa at the Vienna Observatory on 26 September 1914. The carbonaceous C-type asteroid has a poorly determined rotation period of 9.3 hours and seems rather spherical in shape. Any reference of the asteroid's name to a person is unknown. Orbit and classification Fini 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 main-belt at a distance of 2.5–3.0 AU once every 4 years and 7 months (1,665 days; semi-major axis of 2.75 AU). Its orbit has an eccentricity of 0.10 and an inclination of 19° with respect to the ecliptic. The body's observation arc begins at Vienna Observatory on 16 March 1917, where it was officially discovered two and a half years before. Naming "Fini" is an Austrian diminutive of Josephine. Any reference of this minor planet name to a person or occurrence is unknown. Unknown meaning Among the many thousands of named minor planets, Fini 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 Tholen classification, Fini is a common, carbonaceous C-type asteroid. It is also a C-type in the taxonomic classification based on near-infrared colors from the MOVIS-catalog, which was created from data gathered by the VISTA Hemisphere Survey conducted with the VISTA telescope at Paranal Observatory in Chile. Rotation period Several rotational lightcurves of Fini have been obtained from photometric observations. However, the asteroid, which shows a notably low brightness variation – indicative of a spherical rather than elongated shape – still has a poorly determined rotation period. Based on observations from February 2003 and November 2011, Brian Warner at his Palmer Divide Observatory in Colorado, determined three possible period solutions of , and hours with corresponding low amplitudes of , and magnitude (). Petr Pravec and Peter Kušnirák at Ondřejov Observatory derive a rotation period of hours from their observations in October 2001, or half of Warner's period solution, also with an amplitude of 0.2 magnitude (). In September 2010, astronomers at the Palomar Transient Factory in California determined an alternative period of with a brightness variation of 0.06 magnitude (). 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, Fini measures (), () and () kilometers in diameter and its surface has an albedo of (), () and (), respectively. The Collaborative Asteroid Lightcurve Link adopts Petr Pravec's revised WISE-data, that is an albedo of 0.0553 and a diameter of 62.56 kilometers based on an absolute magnitude of 9.78. Alternative mean-diameter measurements published by the WISE team include (), (), (), () and () with corresponding albedos of (), (), (), () and (). On 11 November 2006, an asteroid occultation of Fini gave a best-fit ellipse dimension of () with a low quality rating of 1. 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 000795 Discoveries by Johann Palisa Named minor planets 000795 19140926

3033527

https://en.wikipedia.org/wiki/796%20Sarita

796 Sarita

796 Sarita is a minor planet orbiting the Sun. It was discovered 15 October 1914 by German astronomer Karl W. Reinmuth. This is a main belt that is orbiting at a radius of with a period of and an eccentricity (ovalness) of 0.32. The orbital plane is inclined at an angle of 19.052° from the plane of the ecliptic. Tholen (1989) initially classified it as type XD, although later authors treated it as an M-class body. The object's visual albedo is considered characteristic of the latter type. It has a significantly higher radar albedo than most main belt objects, which also suggests a higher metallic content. References External links 000796 Discoveries by Karl Wilhelm Reinmuth Named minor planets 000796 000796 19141015

3033530

https://en.wikipedia.org/wiki/797%20Montana

797 Montana

797 Montana, provisional designation , is a stony asteroid from the middle region of the asteroid belt, approximately 22 kilometers in diameter. It was discovered on 17 November 1914, by Danish astronomer Holger Thiele at Bergedorf Observatory in Hamburg, Germany. It was later named for the discovering observatory. Classification and orbit Montana is a stony asteroid that orbits the Sun in the middle main-belt at a distance of 2.4–2.7 AU once every 4.04 years (1,474 days). Its orbit has an eccentricity of 0.06 and an inclination of 5° with respect to the ecliptic. The first identification at Heidelberg dates back to 1898 (), while the asteroid's observation arc begins two months after its discovery with the first used observation made at Bergedorf in 1915. Physical characteristics In both the Tholen and SMASS taxonomy, Montana is a common stony S-type asteroid. Rotation period Between 2003 and 2007, three rotational lightcurves of Montana were obtained from photometric observations made by amateur astronomers René Roy, Horacio Correia, Laurent Bernasconi, and Richard Ditteon. All three lightcurves gave a well-defined rotation period of 4.55 hours with a brightness variation between 0.32 and 0.41 magnitude (). Diameter and albedo According to the space-based surveys carried out by the Japanese Akari satellite and NASA's Wide-field Infrared Survey Explorer with its subsequent NEOWISE mission, Montanas surface has an albedo of 0.28–0.35 and its diameter measures between 19.2 and 21.9 kilometers, while the Collaborative Asteroid Lightcurve Link assumes a standard albedo for stony asteroids of 0.20 and calculates a somewhat larger diameter of 25.4 kilometers, as the lower the albedo, the larger the body's diameter at a constant absolute magnitude. Naming This minor planet was named in honor of the Bergedorf Observatory. It was the observatory's first ever made discovery. "Montana" means "mountain village" in Latin and literally translates to "Bergedorf" in German (). 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 000797 Discoveries by Holger Thiele Named minor planets 000797 000797 19141117

3033534

https://en.wikipedia.org/wiki/798%20Ruth

798 Ruth

798 Ruth is a minor planet orbiting the Sun that was discovered by the German astronomer Max Wolf on 21 November 1914. It may have been named after the biblical character Ruth. This main belt asteroid has an orbital period of and is orbiting at a distance of from the Sun with an eccentricity (ovalness) of 0.036. The orbital plane is tilted by 9.2° from the plane of the ecliptic. 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. It is an M-type (metallic) asteroid that displays a significant component of the mineral olivine in its spectrum. 798 Ruth spans and rotates on its axis once every . References External links 000798 Discoveries by Max Wolf Named minor planets 000798 19141121

3033535

https://en.wikipedia.org/wiki/799%20Gudula

799 Gudula

799 Gudula is a minor planet orbiting the Sun discovered by German astronomer Karl Wilhelm Reinmuth on 9 March 1915 at the Heidelberg observatory. Photometric observations of this asteroid at the Oakley Observatory in Terre Haute, Indiana, during 2006 gave a light curve with a period of 14.814 ± 0.003 hours and a brightness variation of 0.30 ± 0.03 in magnitude. References External links 000799 Discoveries by Karl Wilhelm Reinmuth Named minor planets 19150309

3033539

https://en.wikipedia.org/wiki/800%20Kressmannia

800 Kressmannia

800 Kressmannia is an S-type asteroid belonging to the Flora family in the Main Belt. Its rotation period is 4.464 hours. References External links Flora asteroids Kressmannia Kressmannia S-type asteroids (Tholen) 19150320

3035964

https://en.wikipedia.org/wiki/STEP%20%28satellite%29

STEP (satellite)

The Satellite Test of the Equivalence Principle (STEP) is a proposed () space science experiment to test the equivalence principle of general relativity. The experiment is thought to be sensitive enough to test Einstein's theory of gravity and other theories. The basic configuration is that of a drag-free satellite where an outer shell around an inner test mass is used to block solar wind, atmospheric drag, the Earth's magnetic field and other effects which might disturb the motion of a freely-falling inner object. It is designed for an expected sensitivity of one part in 1018. "Research on the STEP accelerometers began in 1971 at Stanford University, and has been supported since 1977 with NASA funding. STEP has been studied twice by ESA at the Phase-A level and has led two other space agencies (CNES and ASI) to study projects aimed at testing the Equivalence Principle in space. STEP is currently undergoing a Phase A study for NASA's office of Space Science Small Explorer program." See also MICROSCOPE (satellite), a similar experiment conducted by CNES References External links Stanford Page STEP: Satellite Test of the Equivalence Principle Benjamin Lange, Experimental Gravitational Physics Using Drag-Free Satellites, (2001) Tests of general relativity Proposed satellites

3036573

https://en.wikipedia.org/wiki/801%20Helwerthia

801 Helwerthia

801 Helwerthia is a C-type asteroid orbiting in the Main belt near the Eunomia family. However, it is not a family member but an un-related interloper in the region because its composition is inconsistent with membership. Its diameter is about 33 km, its albedo around 0.038. An international team of astronomers observed this minor planet photometrically in 2012, determining a rotation period of with an amplitude of in magnitude. References External links 000801 Discoveries by Max Wolf Named minor planets 000801 19150320

3036575

https://en.wikipedia.org/wiki/802%20Epyaxa

802 Epyaxa

802 Epyaxa, provisional designation , is a stony Florian asteroid from the inner regions of the asteroid belt, approximately 7.5 kilometers in diameter. It was discovered by German astronomer Max Wolf at the Heidelberg Observatory in southern Germany, on 20 March 1915. Description The S-type asteroid is a member of the Flora family, one of the largest groups of stony asteroids in the main-belt. It orbits the Sun at a distance of 2.0–2.4 AU once every 3 years and 3 months (1,189 days). Its orbit shows an eccentricity of 0.08 and is tilted by 5 degrees to the plane of the ecliptic. From 2009 to 2014, seven photometric lightcurve analysis rendered a well-defined, concurring rotation period of 4.39 hours (also see adjunct infobox). According to the survey carried out by the U.S. Wide-field Infrared Survey Explorer with its NEOWISE mission, the asteroid's surface has a relatively high albedo of 0.29, while the Collaborative Asteroid Lightcurve Link assumes a more moderate value of 0.24, which is also identical to the albedo of the Flora family's namesake, the asteroid 8 Flora. This minor planet was named after Epyaxa (Ἐπύαξα), wife of King Syennesis and queen of the Kingdom of Cilicia in South Asia Minor in the 5th century BCE. The couple supported the revolt of Cyrus the Younger against his brother Artaxerxes II of Persia, after whom the minor planet 7212 Artaxerxes is named. Epyaxa had her own army and her own lavish budget to spend. Her Kingdom lost its independence and became a Persian satrapy of the Achaemenid Empire after the defeat of Cyrus. References External links Lightcurve plot of 802 Epyaxa, 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 000802 Discoveries by Max Wolf Named minor planets 000802 19150320

3036577

https://en.wikipedia.org/wiki/803%20Picka

803 Picka

803 Picka (prov. designation: or ) is a large and dark background asteroid from the outer regions of the asteroid belt. It was discovered on 21 March 1915, by Austrian astronomer Johann Palisa at the Vienna Observatory. The carbonaceous D-type asteroid has a rotation period of 5.1 hours and measures approximately in diameter. It was named after Czech physician Friedrich Pick (1867–1921). Orbit and classification Picka 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 (2,094 days; semi-major axis of 3.2 AU). Its orbit has an eccentricity of 0.07 and an inclination of 9° with respect to the ecliptic. On 8 July 1899, the asteroid was first observed as at the Boyden Station of the Harvard Observatory in Arequipa, Peru. The body's observation arc begins with its official discovery observation by Johann Palisa at Vienna Observatory on 21 March 1915. Naming This minor planet was named after Czech physician Friedrich Pick (1867–1921) from Prague , who was the first physician to introduce endoscopic methods in medicine. According to the 1917 edition of the astronomical calendar in German "Astronomischer Kalender für 1917", the asteroid was named by friends of the discoverer Johann Palisa. The was mentioned in The Names of the Minor Planets by Paul Herget in 1955 (). Physical characteristics In the SDSS-based taxonomy, Picka is a dark D-type asteroid. In the 1995 SMASS-I survey by Xu, it is classified as an uncommon T-type with some similarities to a D-type (TD). The D-types asteroids are common in the outer main-belt and are very abundant among the Jupiter trojan population. Rotation period In April 2007, a rotational lightcurve of Picka was obtained from photometric observations by French amateur astronomer Pierre Antonini. Lightcurve analysis gave a well-defined rotation period of hours with a high brightness variation of magnitude, indicative of an elongated shape (). Alternative and lower-rated photometric observations were made by Jean-Gabriel Bosch in February 2006, and again by Pierre Antonini in November 2010, which gave a period of and hours with an amplitude of and magnitude (). Lightcurve inversion also modeled the body's shape and poles. In 2013, modelling by an international study using photometric data from the US Naval Observatory, the Uppsala Asteroid Photometric Catalogue, the Palomar Transient Factory and the Catalina Sky Survey gave a concurring sidereal period of hours and two spin axes at (218.0°, 34.0°) and (53.0°, 41.0°) in ecliptic coordinates (λ, β). The body's very elongated shape had already been indicated by the relatively high brightness variation measured during the direct photometric observations. 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), Picka measures (), () and () kilometers in diameter and its surface has an albedo of (), () and (), respectively. The Collaborative Asteroid Lightcurve Link derives an albedo of and a diameter of 46.72 kilometers based on an absolute magnitude of 9.4. On 13 May 2015, an asteroid occultation of Picka gave a best-fit ellipse dimension of (), which is similar to that obtained by the Japanese Akari satellite. These timed observations are taken when the asteroid passes in front of a distant star. This observation still has received a low 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 000803 Discoveries by Johann Palisa Named minor planets 19150321

3036579

https://en.wikipedia.org/wiki/804%20Hispania

804 Hispania

804 Hispania is a minor planet orbiting the Sun. It was discovered from Barcelona (Spain) on 20 March 1915 by Josep Comas Solá (1868–1937), the first asteroid to be discovered by a Spaniard. Hispania is a carbonaceous C-type asteroid. Busarev and Taran (2002) classed it as CP type with a spectrum that shows a highly hydrated body. It has a diameter of 122 kilometers according to measurements made with the W. M. Keck Observatory. This is 30% smaller than the size estimated from the IRAS observatory data. It has a size ratio of 1.16 between its major and minor axes. Two alternate rotation periods have been found for this asteroid: 7.4 hours and double that at 14.8 hours. To explain this discrepancy, it is possible the asteroid has a peculiar shape or it may be a double asteroid. References External links Discovery Circumstances: Numbered Minor Planets (1)-(5000) – Minor Planet Center 000804 Discoveries by Josep Comas Solà Named minor planets 000804 000804 19150320

3036582

https://en.wikipedia.org/wiki/805%20Hormuthia

805 Hormuthia

805 Hormuthia is a minor planet orbiting the Sun. This asteroid follows an elliptical orbit through the main asteroid belt that reaches perihelion just outside the Kirkwood gap at 2.5 AU. Its estimated diameter is 73 km, and it is one of the 500 largest asteroids. 805 Hormuthia was discovered by Max Wolf in 1915, at the University of Heidelberg. The planet is named after Hormuth Kopff, the wife of astronomer August Kopff. References External links List of 500 largest asteroids 000805 Discoveries by Max Wolf Named minor planets 000805 19150417

3036584

https://en.wikipedia.org/wiki/806%20Gyld%C3%A9nia

806 Gyldénia

806 Gyldénia, provisional designation , is a carbonaceous asteroid from the outer region of the asteroid belt, approximately 63 kilometers in diameter. It was discovered on 18 April 1915, by German astronomer Max Wolf at Heidelberg Observatory in southern Germany. The discovery observation was ignored for orbital determination, with the first used observation made at Vienna Observatory on 1 May 2015, reducing the asteroid's observation arc by 2 weeks. The dark C-type asteroid orbits the Sun at a distance of 3.0–3.5 AU once every 5 years and 9 months (2,100 days). Its orbit has an eccentricity of 0.08 and an inclination of 14° with respect to the ecliptic. Several photometric light-curve analysis rendered a rotation period of hours (best result) with a brightness variation of 0.18 in magnitude (). According to the surveys carried out by the Infrared Astronomical Satellite, IRAS, the Japanese Akari satellite, and NASA's Wide-field Infrared Survey Explorer with its subsequent NEOWISE mission, the asteroid's surface has a notably low albedo of less than 0.03, while the Collaborative Asteroid Lightcurve Link derived a somewhat higher value of 0.04. The minor planet was named in honor of the Fenno-Swedish astronomer Hugo Gyldén (1841–1896), who was a director of the Stockholm Observatory. He developed a new technique to calculate the perturbations of planets and comets. The lunar crater Gyldén is also named after the astronomer () 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 000806 Discoveries by Max Wolf Named minor planets 19150418

3036586

https://en.wikipedia.org/wiki/807%20Ceraskia

807 Ceraskia

807 Ceraskia (prov. designation: or ) is an elongated Eos asteroid from the outer regions of the asteroid belt. It was discovered on 18 April 1915, by German astronomer Max Wolf at the Heidelberg-Königstuhl State Observatory in southwest Germany. The S-type asteroid has a rotation period of 7.4 hours and measures approximately in diameter. It was named after Belarusian–Soviet astronomer Vitold Cerasky (1849–1925). Orbit and classification Ceraskia is a core member the Eos family (), the largest asteroid family of the outer main belt consisting of nearly 10,000 known asteroids. It orbits the Sun in the outer asteroid belt at a distance of 2.8–3.2 AU once every 5 years and 3 months (1,913 days; semi-major axis of 3.02 AU). Its orbit has an eccentricity of 0.07 and an inclination of 11° with respect to the ecliptic. The asteroid was first observed as at Heidelberg Observatory on 18 January 1909. The body's observation arc begins at Vienna Observatory on 4 May 1915, or two weeks after its official discovery observation at Heidelberg by Max Wolf. Naming This minor planet was named after Vitold Cerasky (1849–1925), a Belarusian–Soviet astronomer, professor of astronomy at Moscow University and long-time director of the Moscow Observatory . According to Nikolai Chernykh, Cerasky worked extensively on stellar and solar photometry. His name is often transliterated as Vitold Tserasky and Witold Karlovich Ceraski. The lunar crater Tseraskiy is named after him. His wife, Lidiya Tseraskaya (1855–1931), who was also an astronomer, was honored by the crater Tseraskaya on Venus. The was incorrect in the previous three editions of Dictionary of Minor Planet Names, which was based on The Names of the Minor Planets by Paul Herget in 1955 (). Physical characteristics In the Tholen classification, Ceraskia is a common, stony S-type asteroid. In the taxonomic classification based on near-infrared colors from the MOVIS-catalog, the asteroid is a Cgx-subtype that is closest to a carbonaceous C-type and somewhat similar to an uncommon G-type and X-type asteroid. The MOVIS catalog was created from data gather by the VISTA Hemisphere Survey conducted with the VISTA telescope at Paranal Observatory in Chile. Rotation period In October 2017, a rotational lightcurve of Ceraskia was obtained from photometric observations by Matthieu Conjat at Nice Observatory in France. Lightcurve analysis gave a well-defined rotation period of hours with a brightness variation of magnitude (). The result supersedes previous observations by Richard Binzel in April 1983 and by astronomers at the Palomar Transient Factory in California in October 2012, which gave a period of and hours with an amplitude of and magnitude, respectively (). Lightcurve inversion also modeled the body's shape and poles. In 2013, modelling by an international study using photometric data from the US Naval Observatory, the Uppsala Asteroid Photometric Catalogue, the Palomar Transient Factory and the Catalina Sky Survey gave a concurring sidereal period of hours and two spin axes of (325.0°, 23.0°) and (132.0°, 26.0°) in ecliptic coordinates (λ, β). The body's very elongated shape had already been indicated by the relatively high brightness variation measured during the direct photometric observations. 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, Ceraskia measures (), () and () kilometers in diameter and its surface has an albedo of (), () and (), respectively. The Collaborative Asteroid Lightcurve Link derives an albedo of 0.1368 and a diameter of 26.15 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 (). 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 000807 Discoveries by Max Wolf Named minor planets 000807 19150418

3036588

https://en.wikipedia.org/wiki/808%20Merxia

808 Merxia

808 Merxia is a minor planet orbiting the Sun. It forms the namesake for the Merxia family of asteroids that share common orbital elements and physical properties. 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. 808 Merxia is the namesake of the Merxia family of asteroids that share similar orbital elements and physical properties. The members of this family, including 808 Merxia, 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 1662 Hoffmann and 2042 Sitarski. References External links Lightcurve plot of (808) Merxia, Antelope Hills Observatory 000808 Discoveries by Luigi Carnera Named minor planets 000808 19011011

3036590

https://en.wikipedia.org/wiki/809%20Lundia

809 Lundia

809 Lundia is a small, binary, V-type asteroid orbiting within the Flora family in the main belt. It is named after Lund Observatory, Sweden. Characteristics Lundia orbits within the Flora family. However, its V-type spectrum indicates that it is not genetically related to the Flora family, but rather is probably a fragment (two fragments, if its moon is included) ejected from the surface of 4 Vesta by a large impact in the past. Its orbit lies too far from Vesta for it to actually be a member of the Vesta family. It is not clear how it arrived at an orbit so far from Vesta, but other examples of V-type asteroids orbiting fairly far from their parent body are known. A mechanism of interplay between the Yarkovsky effect and nonlinear secular resonances (primarily involving Jupiter and Saturn) has been proposed. Binary system Lightcurve observations in 2005 revealed that Lundia is a binary system of two similarly sized objects orbiting their common centre of gravity. "Lundia" now refers to one of the objects, the other being provisionally designated S/2005 (809) 1. The similarity of size between the two components is suspected because during mutual occultations the brightness drops by a similar amount independently of which component is hidden. Due to the similar size of the primary and secondary the Minor Planet Center lists this as a binary companion. Assuming an albedo similar to 4 Vesta (around 0.4) suggests that the components are about 7 km across. They orbit each other in a period of 15.4 hours, which roughly indicates that the separation between them is very close: to the order of 10–20 km if typical asteroid albedo and density values are assumed. References External links Electronic Telegram No. 239 announcing the binary system (2005 October 1) Discovery Circumstances: Numbered Minor Planets (1)-(5000) – Minor Planet Center (809) Lundia, datasheet, johnstonsarchive.net Asteroids with Satellites, Robert Johnston, johnstonsarchive.net Lightcurve showing signature of the binary 000809 Discoveries by Max Wolf Named minor planets 000809 000809 19150811

3036591

https://en.wikipedia.org/wiki/810%20Atossa

810 Atossa

810 Atossa (prov. designation: or ) is a bright and elongated background asteroid from the region of the Flora family, located in the inner portion of the asteroid belt. It was discovered on 8 September 1915, by German astronomer Max Wolf at the Heidelberg-Königstuhl State Observatory in southern Germany. The presumed S-type asteroid has a rotation period of 4.4 hours and measures approximately in diameter. It was named after the ancient Persian queen Atossa (550–475 BC). Orbit and classification Atossa is a non-family asteroid of the main belt's background population when applying the synthetic hierarchical clustering method (HCM) by Nesvorný to its proper orbital elements. However, in an older HCM-analysis by Zappalà from 1995, this asteroid is considered a member of the Flora family (), a giant asteroid family and the largest family of stony asteroids in the main-belt. In a third HCM-analysis by Milani and Knežević (AstDyS), it is also a background asteroid, as this analysis does not recognize the Flora asteroid clan as a proper family. Atossa orbits the Sun in the inner asteroid belt at a distance of 1.8–2.6 AU once every 3 years and 3 months (1,174 days; semi-major axis of 2.18 AU). Its orbit has an eccentricity of 0.18 and an inclination of 3° with respect to the ecliptic. The body's observation arc begins at Heidelberg Observatory with its official discovery observation on 8 September 1915. Naming This minor planet was named after Atossa (550–475 BC), an ancient Persian queen, daughter of Cyrus, wife of Darius. The was also mentioned in The Names of the Minor Planets by Paul Herget in 1955 (). The asteroids 7209 Cyrus and 7210 Darius were named after her father and husband, respectively. Physical characteristics Atossa is an assumed, stony S-type asteroid, based on its high albedo (see below) and its proximity or potential membership to the stony Flora family. Rotation period In August 2005, a rotational lightcurve of Atossa was obtained from photometric observations by French amateur astronomer Philippe Baudoin. Lightcurve analysis gave a well-defined rotation period of hours with a high brightness variation of magnitude, indicative of a non-spherical, elongated shape (). 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 (12.0°, 67.0°) and (188.0°, 69.0°) 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, Atossa measures kilometers in diameter and its surface has an albedo of . The Collaborative Asteroid Lightcurve Link assumes a standard albedo for a Florian asteroid of 0.24 and calculates a diameter of 8.58 kilometers based on an absolute magnitude of 12.5. 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 000810 Discoveries by Max Wolf Named minor planets 19150908

3036594

https://en.wikipedia.org/wiki/811%20Nauheima

811 Nauheima

811 Nauheima is a minor planet orbiting the Sun. It was named after Bad Nauheim, a spa town in western Germany. References External links 000811 Discoveries by Max Wolf Named minor planets 000811 19150908

3036597

https://en.wikipedia.org/wiki/813%20Baumeia

813 Baumeia

813 Baumeia (prov. designation: or ) is a stony background asteroid from the inner regions of the asteroid belt. It was discovered on 28 November 1915, by German astronomer Max Wolf at the Heidelberg Observatory in southwest Germany. The common S-type asteroid has a rotation period of 10.5 hours and measures approximately in diameter. It was named for H. Baum, a German student of astronomy at Heidelberg who was killed in World War I. Orbit and classification Baumeia 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 2.2–2.3 AU once every 3 years and 4 months (1,211 days; semi-major axis of 2.22 AU). Its orbit has an eccentricity of 0.03 and an inclination of 6° with respect to the ecliptic. The body's observation arc begins with its first observation as at Heidelberg on 4 April 1907, more than 8 years prior to its official discovery observation. Naming This minor planet was named im memory of H. Baum, a German astronomy student at Heidelberg University who was in World War I. The naming was published in the journal Astronomische Nachrichten in 1921 (AN 214, 69). The was also mentioned in The Names of the Minor Planets by Paul Herget in 1955 (). Physical characteristics Baumeia is a common, stony S-type asteroid in both the SMASS-I taxonomy by Xu (1995), as well as in the taxonomic classification based on MOVIS near-infrared colors from the catalog of the VISTA Hemisphere Survey conducted with the VISTA telescope at Paranal Observatory in Chile. Rotation period In January 2019, a rotational lightcurve of Baumeia was obtained from photometric observations by European astronomers Bruno Christmann, Raoul Behrend, Anaël Wünsche, Marc Bretton, Rui Goncalves, Josep Bosch. Lightcurve analysis gave a well-defined rotation period of hours with a brightness variation of magnitude (). The result confirms and refines previous observations by French amateur astronomer René Roy in February 2003, which gave a period of hours with an amplitude of magnitude (), by Jean-Gabriel Bosch at the French Collonges Observatory in February 2006, which gave an identical period of hours with an amplitude of magnitude (), by James W. Brinsfield at the Via Capote Observatory in Australia in November 2008, which gave the first secured 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) and the Infrared Astronomical Satellite IRAS, Baumeia measures () and () kilometers in diameter and its surface has an albedo of () and (), respectively. The Collaborative Asteroid Lightcurve Link derives an albedo of 0.2396 and a diameter of 13.61 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 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 000813 Discoveries by Max Wolf Named minor planets 19151128

3036599

https://en.wikipedia.org/wiki/814%20Tauris

814 Tauris

814 Tauris (prov. designation: or ) is a dark and very large background asteroid, approximately in diameter, located the outer regions of the asteroid belt. It was discovered on 2 January 1916, by astronomer Russian Grigory Neujmin at the Simeiz Observatory on Crimea. The carbonaceous C-type asteroid has a longer-than average rotation period of 35.8 hours. It was named after the ancient name of the Crimean peninsula where the discovering observatory is located. Orbit and classification Tauris 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 2.2–4.1 AU once every 5 years and 7 months (2,048 days; semi-major axis of 3.16 AU). Its orbit has a notably high eccentricity of 0.31 and an inclination of 22° with respect to the ecliptic. This gives it a TJupiter of 3.0250, near the boundary of 3, which separates asteroids (above 3) from the Jupiter-family comets (below 3). Tauris was first observed as at Taunton Observatory on 12 May 1907. The body's observation arc begins at Heidelberg Observatory on 30 January 1916, or four weeks after its official discovery observation at Simeiz Observatory. Naming This minor planet was named after the ancient name of the Crimean peninsula, Tauris. Lutz Schmadel, the author of the Dictionary of Minor Planet Names also mentions a mountain with the same name on the southwest coast of Crimea. In addition, Baltic German astronomer Ludwig von Struve (1858–1920) also taught astronomy at the Tavrida University (Tauris University) in Simferopol, a large city on the Crimean peninsula (R. Bremer). The was also mentioned in The Names of the Minor Planets by Paul Herget in 1955 (). Physical characteristics In the Tholen classification as well in the Bus–Binzel SMASS classification, Tauris is a common, carbonaceous C-type asteroid, while in both the Tholen- and SMASS-like taxonomy of the Small Solar System Objects Spectroscopic Survey (S3OS2), it is an X-type asteroid. Rotation period In 1983, a rotational lightcurve of Tauris, obtained from photometric observations with the ESO 0.5-metre telescope at La Silla, Chile, was by published by Belgian astronomer Henri Debehogne in collaboration with Italian astronomers Giovanni de Sanctis and Vincenzo Zappalà. Lightcurve analysis gave a rotation period of hours with a brightness variation of magnitude (). In May 2013, Michael S. Alkema at the Elephant Head Observatory in Arizona determined an identical 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, Tauris 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 0.0470 and a diameter of 109.56 kilometers based on an absolute magnitude of 8.74. Alternative mean-diameter measurements published by the WISE team include (), (), () and () with corresponding albedos of (), (), () and (). Several asteroid occultations of Tauris were observed between 1999 and 2015. These timed observations are taken when the asteroid passes in front of a distant star. The two best-rated observations made on 26 and 29 July 2015, gave a best-fit ellipse dimension of () and (), respectively. However, these two observations still received a relatively poor quality rating. 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 000814 Discoveries by Grigory Neujmin Named minor planets 000814 000814 19160102

3036600

https://en.wikipedia.org/wiki/815%20Coppelia

815 Coppelia

815 Coppelia is a minor planet orbiting the Sun that was discovered by German astronomer Max Wolf on 2 February 1916 from Heidelberg named after Coppélia, a comic ballet. Photometric observations of this asteroid at the Rozhen Observatory in Bulgaria during 2010 gave a light curve with a period of 4.4565 hours and a brightness variation of 0.24 in magnitude. This is consistent with a period of 4.421 hours and an amplitude of 0.27 obtained during a 2006 study. References External links 000815 Discoveries by Max Wolf Named minor planets 000815 19160202

3036602

https://en.wikipedia.org/wiki/816%20Juliana

816 Juliana

816 Juliana is a minor planet orbiting the Sun. It measures 59.85k in diameter. It was discovered on 8 February 1916 by Max Wolf at the Landessternwarte Heidelberg-Königstuhl Observatory in Heidelberg, Germany. Wolf probably chose the name to honour Princess Juliana (later Queen Juliana of the Netherlands); he had previously named 392 Wilhelmina after her mother. References External links 000816 Discoveries by Max Wolf Named minor planets 19160208

3036603

https://en.wikipedia.org/wiki/817%20Annika

817 Annika

817 Annika (prov. designation: or ) is a background asteroid in the region of the Eunomia family, located in the central portion of the asteroid belt. It was discovered on 6 February 1916, by German astronomer Max Wolf at the Heidelberg-Königstuhl State Observatory in southwest Germany. The stony S-type asteroid (Sl) has a rotation period of 10.56 hours and measures approximately in diameter. Any reference of the asteroid's name to a person is unknown. Orbit and classification Annika is a non-family asteroid of the main belt's background population when applying the hierarchical clustering method (HCM) to its proper orbital elements by Nesvorný as well as by Milani and Knežević (AstDyS). In the 1995 HCM-analysis by Zappalà, however, Annika is a member of the Eunomia family (), a prominent family of stony asteroids and the largest one in the intermediate main belt with more than 5,000 members. It orbits the Sun in the central main-belt at a distance of 2.1–3.1 AU once every 4 years and 2 months (1,523 days; semi-major axis of 2.59 AU). Its orbit has an eccentricity of 0.18 and an inclination of 11° with respect to the ecliptic. The body's observation arc begins with its official discovery observation at Heidelberg Observatory on 6 February 1916. Naming "Annika" is a common German feminine given name. Any reference to a person or occurrence for the naming of this minor planet is unknown. Unknown meaning Among the many thousands of named minor planets, Annika 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 Tholen-like taxonomy of the Small Solar System Objects Spectroscopic Survey (S3OS2), Annika is a common, stony S-type asteroid, while in the SMASS-like taxonomic variant of the S3OS2 survey, it is an Sl-subtype which transitions from the S-type to the uncommon L-type asteroid. Rotation period In October 2002, a rotational lightcurve of Annika was obtained from photometric observations by Colin Bembrick at Mount Tarana Observatory , Australia, in collaboration with Greg Bolt and Tom Richards near Perth and Melbourne, respectively. Lightcurve analysis gave a well-defined rotation period of hours with a brightness variation of magnitude (). This period was confirmed by Gérald Rousseau in March 2012, who determined a very similar period of hours with an amplitude of magnitude (). 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, Annika measures (), () and () kilometers in diameter and its surface has an albedo of (), () and (), respectively. The Collaborative Asteroid Lightcurve Link derives an albedo of 0.2062 and a diameter of 22.20 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 (). On 26 August 2010, an asteroid occultation of Annika gave a best-fit ellipse dimension of (). 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 000817 Discoveries by Max Wolf Named minor planets 000817 19160206

3036605

https://en.wikipedia.org/wiki/818%20Kapteynia

818 Kapteynia

818 Kapteynia is a minor planet orbiting the Sun. This asteroid is named for the Dutch astronomer Jacobus Kapteyn. References External links 000818 Discoveries by Max Wolf Named minor planets 19160221

3036607

https://en.wikipedia.org/wiki/819%20Barnardiana

819 Barnardiana

819 Barnardiana is a minor planet orbiting the Sun, discovered on March 3, 1916, by the German astronomer Max Wolf in Heidelberg. References External links 000819 Discoveries by Max Wolf Named minor planets 000819 19160303

3036610

https://en.wikipedia.org/wiki/821%20Fanny

821 Fanny

821 Fanny (prov. designation: or ) is a dark background asteroid and slow rotator from the central regions of the asteroid belt. It was discovered on 31 March 1916, by German astronomer Max Wolf at the Heidelberg-Königstuhl State Observatory in southwest Germany. The carbonaceous C-type asteroid (Ch) has an exceptionally long rotation period of 236.6 hours and measures approximately in diameter. Any reference of the asteroid's name to a person is unknown. Orbit and classification Fanny 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 2.2–3.4 AU once every 4 years and 7 months (1,686 days; semi-major axis of 2.77 AU). Its orbit has an eccentricity of 0.21 and an inclination of 5° with respect to the ecliptic. The body's observation arc begins at the Heidelberg Observatory on 1 April 1916, with its first recorded observation, the night after its official discovery. 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, Fanny 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 Tholen classification and in the SDSS-based taxonomy, Fanny is a common, carbonaceous C-type asteroid. In the Bus–Binzel SMASS classification, it is a hydrated carbonaceous Ch-subtype. Rotation period In 2018, from April to June, a rotational lightcurve of Fanny was obtained from photometric observations over 46 nights by Frederick Pilcher at the Organ Mesa Observatory in New Mexico. Analysis gave a bimodal lightcurve with a rotation period of hours and a brightness variation of magnitude (). This determination was adopted by the Lightcurve Data base and accounts for Pilcher's observations taken between April and May. For observations taken between May and June, a similar period of hours with a somewhat higher amplitude of magnitude was derived (). The observer also ruled out non-principal axis rotation ("tumblin"), and considers a double period 470 hours as very unlikely. This makes it a slow rotator, as most asteroids have much shorter periods between 2 and 20 hours. , Fanny ranks among the 250th slowest rotator known to exist. During the same apparition, Tom Polakis at the Command Module Observatory in Arizona obtained a somewhat longer period of hours with a brightness variation of magnitude (). The result supersedes an incorrect period of hours with an amplitude of magnitude from a tentative one-night observation by French amateur astronomers Paul Krafft, Olivier Gerteis, Hubert Gully, Luc Arnold and Matthieu Bachschmidt from 2013 (). 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), Fanny 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 C-type asteroid of 0.057 and calculates a diameter of 23.86 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 (). 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 000821 Discoveries by Max Wolf Named minor planets 000821 000821 19160331

3036612

https://en.wikipedia.org/wiki/820%20Adriana

820 Adriana

820 Adriana, provisional designation 1916 ZB, is an exceptionally dark asteroid from the outer region of the asteroid belt, about 59 kilometers in diameter. It was discovered by German astronomer Max Wolf at Heidelberg Observatory in southern Germany, on 30 March 1916. The asteroid orbits the Sun at a distance of 3.0–3.3 AU once every 5 years and 7 months (2,027 days). Its orbit shows an eccentricity of 0.05 and is tilted by 6 degrees to the plane of the ecliptic. According to the survey carried out by the Infrared Astronomical Satellite, IRAS, the asteroid's surface has an extremely low albedo of 0.02. The body's spectral type remains unknown, as does its rotation period. By 2014, there were only 22 asteroids with an unknown rotation period for the low-numbered asteroids up to number 1000 (also see 398 Admete). Any reference of this name to a person or occurrence is unknown. 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 000820 Discoveries by Max Wolf Named minor planets 19160330

3036613

https://en.wikipedia.org/wiki/822%20Lalage

822 Lalage

822 Lalage (prov. designation: or ) is a background asteroid from the inner regions of the asteroid belt. It was discovered on 31 March 1916, by astronomer Max Wolf at the Heidelberg-Königstuhl State Observatory in southwest Germany. The likely highly elongated asteroid with an unclear spectral type has a short rotation period of 3.3 hours and measures approximately in diameter. Any reference to the origin of the asteroid's name is unknown. Orbit and classification Lalage 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 1.9–2.6 AU once every 3 years and 5 months (1,237 days; semi-major axis of 2.26 AU). Its orbit has an eccentricity of 0.16 and an inclination of 1° with respect to the ecliptic. The body's observation arc begins at the Bergedorf Observatory on 6 April 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 minor planets, Lalage 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, Lalage has an unusual spectrum, that is closest to a dark D-type, somewhat similar to an X-type, and, to a lesser extent, a carbonaceous C-type asteroid. Conversely, the Small Solar System Objects Spectroscopic Survey (S3OS2), classifies the body an uncommon A-type in the survey's Tholen-like taxonomic variant, and as an Sl-subtype – which transitions from the stony S-type to the uncommon L-type asteroid – in its SMASS-like variant. Rotation period In September 1992, a rotational lightcurve of Lalage was obtained from photometric observations by Polish astronomer Wiesław Wiśniewski. Lightcurve analysis gave a short rotation period of hours with a high brightness variation of magnitude, indicative of a non-spherical, elongated shape (). Since then, additional period determinations gave hours with an amplitude of magnitude () by David Higgins in October 2009, hours with an amplitude of magnitude () by Robert Stephens in January 2014, and hours with an amplitude of magnitude () by Daniel A. Klinglesmith in February 2014. A modeled lightcurves using photometric data from the BlueEye600 robotic telescope at Ondřejov Observatory gave a sidereal period of . The modelling also gave two poles at (343.0°, −74.0°) and (133.0°, −75.0°) 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 and the Japanese Akari satellite, Lalage measures () and () kilometers in diameter and its surface has an albedo of () and (), respectively. The Collaborative Asteroid Lightcurve Link assumes an albedo of 0.20 and a diameter of 10.16 kilometers based on an absolute magnitude of 12.33. 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 Discovery Circumstances: Numbered Minor Planets (1)-(5000) – Minor Planet Center 000822 Discoveries by Max Wolf Named minor planets 000822 19160331

3036614

https://en.wikipedia.org/wiki/823%20Sisigambis

823 Sisigambis

823 Sisigambis is an asteroid belonging to the Flora family in the Main Belt. Its diameter is about 17 km and it has an albedo of 0.179. Its rotation period is unknown but appears to be greater than at least 12 hours. The asteroid is named after Sisygambis, the mother of Darius III of Persia. References External links 000823 Discoveries by Max Wolf Named minor planets 000823 19160331