810 Atossa

810 Atossa (prov. designation: A915 RS or 1915 XQ) is a bright and elongated background asteroid from the region of the Flora family, located 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 8 kilometers (5 miles) in diameter. It was named after the ancient Persian queen Atossa (550–475 BC).[3]

810 Atossa
Shape model of Atossa from its lightcurve
Discovery [1]
Discovered byM. F. Wolf
Discovery siteHeidelberg Obs.
Discovery date8 September 1915
Designations
(810) Atossa
Pronunciation/əˈtɒsə/[2]
Named after
Atossa (550–475 BC)
(Persian queen)[3]
A915 RS · 1931 PF
1934 NB · 1947 PA
1915 XQ
Orbital characteristics [4]
Epoch 31 May 2020 (JD 2459000.5)
Uncertainty parameter 0
Observation arc104.41 yr (38,136 d)
Aphelion2.5717 AU
Perihelion1.7853 AU
2.1785 AU
Eccentricity0.1805
3.22 yr (1,174 d)
198.29°
0° 18m 23.4s / day
Inclination2.6122°
152.69°
195.84°
Physical characteristics
Mean diameter
8.104±0.119 km[8][9]
4.3851±0.0004 h[10][11]
  • (12.0°, 67.0°) (λ1/β1)[12]
  • (188.0°, 69.0°) (λ2/β2)[12]
0.224±0.046[8][9]
S (assumed)[10]

    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.[6] However, in an older HCM-analysis by Zappalà from 1995,[7] this asteroid is considered a member of the Flora family (402), a giant asteroid family and the largest family of stony asteroids in the main-belt.[13]:23 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.[5]

    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.[4] 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 naming was also mentioned in The Names of the Minor Planets by Paul Herget in 1955 (H 80).[3] 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,[10] based on its high albedo (see below) and its proximity or potential membership to the stony Flora family.[7][13]:23

    Lightcurve-based 3D-model of Atossa

    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 4.3851±0.0004 hours with a high brightness variation of 0.55±0.01 magnitude, indicative of a non-spherical, elongated shape (U=3).[11]

    In 2011, a modeled lightcurve using data from the Uppsala Asteroid Photometric Catalogue (UAPC) and other sources gave a sidereal period 4.38547±0.00005 hours, as well as two spin axes at (12.0°, 67.0°) and (188.0°, 69.0°) in ecliptic coordinates (λ, β).[12]

    Diameter and albedo

    According to the survey carried out by the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer, Atossa measures 8.104±0.119 kilometers in diameter and its surface has an albedo of 0.224±0.046.[8] 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.[10] Alternative mean-diameter measurements published by the WISE team include (6.99±1.24 km) and (8.356±0.053 km) with corresponding albedos of (0.35±0.17) and (0.2115±0.0097).[10]

    gollark: You do need to wait for messages before sending a few.
    gollark: Okay, detecting those things ought to be doable.
    gollark: How are if statements going to help us?
    gollark: We could program in general complaints like "lol no types".
    gollark: A great idea. But how will it know what aspect of someone's code to snark about?

    References
    1. "810 Atossa (A915 RS)". Minor Planet Center. Retrieved 26 March 2020.
    2. Noah Webster (1884) A Practical Dictionary of the English Language
    3. Schmadel, Lutz D. (2007). "(810) Atossa". Dictionary of Minor Planet Names. Springer Berlin Heidelberg. p. 75. doi:10.1007/978-3-540-29925-7_811. ISBN 978-3-540-00238-3.
    4. "JPL Small-Body Database Browser: 810 Atossa (A915 RS)" (2020-02-05 last obs.). Jet Propulsion Laboratory. Retrieved 26 March 2020.
    5. "Asteroid 810 Atossa – Proper Elements". AstDyS-2, Asteroids – Dynamic Site. Retrieved 26 March 2020.
    6. "Asteroid 810 Atossa". Small Bodies Data Ferret. Retrieved 26 March 2020.
    7. Zappalà, V.; Bendjoya, Ph.; Cellino, A.; Farinella, P.; Froeschle, C. (1997). "Asteroid Dynamical Families". NASA Planetary Data System: EAR-A-5-DDR-FAMILY-V4.1. Retrieved 26 March 2020.} (PDS main page)
    8. Mainzer, A. K.; Bauer, J. M.; Cutri, R. M.; Grav, T.; Kramer, E. A.; Masiero, J. R.; et al. (June 2016). "NEOWISE Diameters and Albedos V1.0". NASA Planetary Data System. Bibcode:2016PDSS..247.....M. Retrieved 26 March 2020.
    9. Masiero, Joseph R.; Grav, T.; Mainzer, A. K.; Nugent, C. R.; Bauer, J. M.; Stevenson, R.; et al. (August 2014). "Main-belt Asteroids with WISE/NEOWISE: Near-infrared Albedos". The Astrophysical Journal. 791 (2): 11. arXiv:1406.6645. Bibcode:2014ApJ...791..121M. doi:10.1088/0004-637X/791/2/121.
    10. "LCDB Data for (810) Atossa". Asteroid Lightcurve Database (LCDB). Retrieved 26 March 2020.
    11. Behrend, Raoul. "Asteroids and comets rotation curves – (810) Atossa". Geneva Observatory. Retrieved 26 March 2020.
    12. Hanuš, J.; Ďurech, J.; Brož, M.; Warner, B. D.; Pilcher, F.; Stephens, R.; et al. (June 2011). "A study of asteroid pole-latitude distribution based on an extended set of shape models derived by the lightcurve inversion method". Astronomy and Astrophysics. 530: A134. arXiv:1104.4114. Bibcode:2011A&A...530A.134H. doi:10.1051/0004-6361/201116738. ISSN 0004-6361.
    13. Nesvorný, D.; Broz, M.; Carruba, V. (December 2014). "Identification and Dynamical Properties of Asteroid Families". Asteroids IV: 297–321. arXiv:1502.01628. Bibcode:2015aste.book..297N. doi:10.2458/azu_uapress_9780816532131-ch016.
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