810 Atossa
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810 Atossa (prov. designation: Template:Mp or Template:Mp) 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.[1] The presumed S-type asteroid has a rotation period of 4.4 hours and measures approximately Script error: No such module "convert". in diameter. It was named after the ancient Persian queen Atossa (550–475 BC).[2]
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.[3] However, in an older HCM-analysis by Zappalà from 1995,[4] this asteroid is considered a member of the Flora family (402Script error: No such module "Check for unknown parameters".), a giant asteroid family and the largest family of stony asteroids in the main-belt.[5]Template:Rp 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.[6]
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.[7] The body's observation arc begins at Heidelberg Observatory with its official discovery observation on 8 September 1915.[1]
Naming
This minor planet was named after Atossa (550–475 BC), an ancient Persian queen, daughter of Cyrus, wife of Darius. The Template:MoMP was also mentioned in The Names of the Minor Planets by Paul Herget in 1955 (H 80Script error: No such module "Check for unknown parameters".).[2] The asteroids 7209 Cyrus and 7210 Darius were named after her father and husband, respectively.Script error: No such module "Unsubst".
Physical characteristics
Atossa is assumed to be a stony S-type asteroid,[8] based on its high albedo (see below) and its proximity or potential membership to the stony Flora family.[4][5]Template:Rp
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 Script error: No such module "val". hours with a high brightness variation of Script error: No such module "val". magnitude, indicative of a non-spherical, elongated shape (U=3Script error: No such module "Check for unknown parameters".).[9]
In 2011, a modeled lightcurve using data from the Uppsala Asteroid Photometric Catalogue (UAPC) and other sources gave a sidereal period of Script error: No such module "val". hours, as well as two spin axes at (12.0°, 67.0°) and (188.0°, 69.0°) in ecliptic coordinates (λ, β).[10]
Diameter and albedo
According to the survey carried out by the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer, Atossa measures Script error: No such module "val". kilometers in diameter and its surface has an albedo of Script error: No such module "val"..[11] 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.[8] Alternative mean diameter measurements published by the WISE team include (Script error: No such module "val".) and (Script error: No such module "val".) with corresponding albedos of (Script error: No such module "val".) and (Script error: No such module "val".).[8]
References
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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
- Template:AstDys
- Template:PAGENAMEBASE at the JPL Small-Body DatabaseTemplate:EditAtWikidata
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