1022 Olympiada

1022 Olympiada, provisional designation 1924 RT, is a background asteroid from the central regions of the asteroid belt, approximately 30 kilometers (19 miles) in diameter. It was discovered at the Simeiz Observatory on the Crimean peninsula on 23 June 1924, by Soviet astronomer Vladimir Albitsky,[1] who named it after his mother, Olimpiada Albitskaya.[2] The X-type asteroid has a short rotation period of 3.83 hours.[4]

1022 Olympiada
Shape model of Olympiada from its lightcurve
Discovery [1]
Discovered byV. Albitzkij
Discovery siteSimeiz Obs.
Discovery date23 June 1924
Designations
(1022) Olympiada
Named after
Olimpiada Albitskaya [2]
(discoverer's mother)
1924 RT · 1928 FQ
1948 QO · 1957 OC
1961 JF · 1962 QK
A910 NA
main-belt [1][3] · (outer) [4]
background [5]
Orbital characteristics [3]
Epoch 23 March 2018 (JD 2458200.5)
Uncertainty parameter 0
Observation arc106.79 yr (39,006 d)
Aphelion3.2959 AU
Perihelion2.3144 AU
2.8051 AU
Eccentricity0.1749
4.70 yr (1,716 d)
10.487°
0° 12m 35.28s / day
Inclination21.054°
111.97°
124.74°
Physical characteristics
Mean diameter
26.39±2.2 km[6]
26.65 km (derived)[4]
32.88±0.76 km[7]
34.30±0.99 km[8]
3.822±0.006 h[9]
3.833±0.005 h[10][lower-alpha 1]
3.8331±0.0006 h[11]
3.83359±0.00005 h[12]
3.834±0.001 h[13]
3.835±0.0016 h[14]
4.589±0.002 h (retracted)[15]
0.105±0.005[7]
0.125±0.017[8]
0.1600±0.030[6]
0.2069 (derived)[4]
SMASS = X [3][4]
10.053±0.001 (R)[14]
10.20[3][4][8]
10.46±0.26[16]
10.50[6][7]

    Orbit and classification

    Olympiada is a non-family asteroid from the main belt's background population.[5] It orbits the Sun in the central asteroid belt at a distance of 2.3–3.3 AU once every 4 years and 8 months (1,716 days; semi-major axis of 2.81 AU). Its orbit has an eccentricity of 0.17 and an inclination of 21° with respect to the ecliptic.[3]

    The body's observation arc begins with its first observation as A910 NA at Heidelberg Observatory in July 1910, or nearly 14 years prior to its official discovery observation at Simeiz.[1]

    Naming

    This minor planet was named after Olimpiada Albitskaya, mother of the discoverer Vladimir Albitsky (1891–1952).[2] No accurate naming citation was given for this asteroid in The Names of the Minor Planets. The author of the Dictionary of Minor Planets, Lutz Schmadel, learned about the naming circumstances from Nikolai Chernykh (1931–2004), a prolific long-time astronomer at Nauchnij, Crimea.[2]

    Physical characteristics

    In the SMASS classification, Olympiada is an X-type asteroid.[3][4]

    Rotation period

    Several rotational lightcurves of Olympiada have been obtained from photometric observations by American astronomer Brian Warner at his Palmer Divide Observatory in Colorado. Analysis of the best-rated lightcurve from April 2008 gave a rotation period of 3.833 hours with a consolidated brightness variation between 0.27 and 0.66 magnitude (U=3),[4][10][lower-alpha 1] while the period of his first 1999-observation was later revised from 4.589 to 3.822 hours.[9][15] For an asteroid of its size, it has a rather fast spin-rate.

    This period is also in good agreement with other observations obtained by astronomers at the Belgrade Astronomical Observatory (3.8331 h; Δ0.35 mag) in March 2008, by astronomers at the Palomar Transient Factory (3.835 h; Δ0.46 mag) in January 2012, and by a group of Italian astronomers (3.834 h; Δ0.66 mag) in March 2017 (U=3/2/3).[11][13][14]

    Poles

    In 2011, a modeled lightcurve using data from the Uppsala Asteroid Photometric Catalogue and other sources gave a concurring sidereal period 3.83359 hours, as well as two poles at (46.0°, 10.0°) and (242.0°, 52.0°) in ecliptic coordinates (λ, β) (Q=2+).[12] Brian Warner also determined two spin axes at (40.0°, 18.0°) and (250.0°, 71.0°) using his data set from 2008 (Q=2).[9]

    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, Olympiada measures between 26.39 and 34.30 kilometers in diameter and its surface has an albedo between 0.105 and 0.1600.[6][7][8]

    The Collaborative Asteroid Lightcurve Link derives an untypically high albedo of 0.2069 and a diameter of 26.65 kilometers based on an absolute magnitude of 10.2.[4]


    Notes
    1. Lightcurve plot of (1022) Olympiada, Palmer Divide Observatory, B. D. Warner (2008). Rotation period 3.833±0.006 hours with a brightness amplitude of 0.34±0.02 mag. Quality code of 3. Summary figures at the LCDB
    gollark: Well, it or the newer models.
    gollark: 512-bit CPU, 3EB memory, 10¹¹ pins, RGB lighting, 1222YHz clocks, 6-layer nested power management processors, 1Tbps Ethernet. It's great and all are to have it.
    gollark: It's last³ month's GTech™ GCIS02-2027 microcontroller.
    gollark: <@!559418497734803470> IMMEDIATELY undergo 0 to 6 of the linear transformations described in the G🐝🐝512<:bismuth:810276089565806644>666FC-4A manual.
    gollark: Fearsome.

    References
    1. "1022 Olympiada (1924 RT)". Minor Planet Center. Retrieved 15 March 2018.
    2. Schmadel, Lutz D. (2007). "(1022) Olympiada". Dictionary of Minor Planet Names. Springer Berlin Heidelberg. p. 88. doi:10.1007/978-3-540-29925-7_1023. ISBN 978-3-540-00238-3.
    3. "JPL Small-Body Database Browser: 1022 Olympiada (1924 RT)" (2017-04-30 last obs.). Jet Propulsion Laboratory. Retrieved 15 March 2018.
    4. "LCDB Data for (1022) Olympiada". Asteroid Lightcurve Database (LCDB). Retrieved 15 March 2018.
    5. "Asteroid 1022 Olympiada – Nesvorny HCM Asteroid Families V3.0". Small Bodies Data Ferret. Retrieved 24 October 2019.
    6. Tedesco, E. F.; Noah, P. V.; Noah, M.; Price, S. D. (October 2004). "IRAS Minor Planet Survey V6.0". NASA Planetary Data System. 12: IRAS-A-FPA-3-RDR-IMPS-V6.0. Bibcode:2004PDSS...12.....T. Retrieved 22 October 2019.
    7. Usui, Fumihiko; Kuroda, Daisuke; Müller, Thomas G.; Hasegawa, Sunao; Ishiguro, Masateru; Ootsubo, Takafumi; et al. (October 2011). "Asteroid Catalog Using Akari: AKARI/IRC Mid-Infrared Asteroid Survey". Publications of the Astronomical Society of Japan. 63 (5): 1117–1138. Bibcode:2011PASJ...63.1117U. doi:10.1093/pasj/63.5.1117. Retrieved 17 October 2019. (online, AcuA catalog p. 153)
    8. Masiero, Joseph R.; Mainzer, A. K.; Grav, T.; Bauer, J. M.; Cutri, R. M.; Nugent, C.; et al. (November 2012). "Preliminary Analysis of WISE/NEOWISE 3-Band Cryogenic and Post-cryogenic Observations of Main Belt Asteroids". The Astrophysical Journal Letters. 759 (1): 5. arXiv:1209.5794. Bibcode:2012ApJ...759L...8M. doi:10.1088/2041-8205/759/1/L8. Retrieved 15 March 2018.
    9. Warner, Brian D.; Durech, Josef; Fauerbach, Michael; Marks, Scott (October 2008). "Shape and Spin Models for Four Asteroids". The Minor Planet Bulletin. 35 (4): 167–171. Bibcode:2008MPBu...35..167W. ISSN 1052-8091. Retrieved 15 March 2018.
    10. Warner, Brian D. (June 2005). "Revised lightcurve analysis for 1022 Olympiada and 3285 Ruth Wolfe". The Minor Planet Bulletin. 32 (2): 26. Bibcode:2005MPBu...32...26W. ISSN 1052-8091. Retrieved 15 March 2018.
    11. Benishek, Vladimir; Protitch-Benishek, Vojislava (April 2009). "CCD Photometry of Asteroids at the Belgrade Astronomical Observatory: 2008 January-September". The Minor Planet Bulletin. 36 (2): 35–37. Bibcode:2009MPBu...36...35B. ISSN 1052-8091. Retrieved 15 March 2018.
    12. Hanus, J.; Durech, J.; Broz, 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 & Astrophysics. 530: 16. arXiv:1104.4114. Bibcode:2011A&A...530A.134H. doi:10.1051/0004-6361/201116738. Retrieved 15 March 2018.
    13. Franco, Lorenzo; Baj, Giorgio; Tinella, Vito; Bachini, Mauro; Succi, Giacomo; Casalnuovo, Giovanni Battista; et al. (October 2017). "Rotation Periods for Three Main-belt Asteroids". The Minor Planet Bulletin. 44 (4): 311–312. Bibcode:2017MPBu...44..311F. ISSN 1052-8091. Retrieved 15 March 2018.
    14. Waszczak, Adam; Chang, Chan-Kao; Ofek, Eran O.; Laher, Russ; Masci, Frank; Levitan, David; et al. (September 2015). "Asteroid Light Curves from the Palomar Transient Factory Survey: Rotation Periods and Phase Functions from Sparse Photometry". The Astronomical Journal. 150 (3): 35. arXiv:1504.04041. Bibcode:2015AJ....150...75W. doi:10.1088/0004-6256/150/3/75. Retrieved 15 March 2018.
    15. Warner, B. D. (December 1999). "Asteroid Photometry at the Palmer Divide Observatory". The Minor Planet Bulletin. 26.: 31. Bibcode:1999MPBu...26...31W. Retrieved 15 March 2018.
    16. Veres, Peter; Jedicke, Robert; Fitzsimmons, Alan; Denneau, Larry; Granvik, Mikael; Bolin, Bryce; et al. (November 2015). "Absolute magnitudes and slope parameters for 250,000 asteroids observed by Pan-STARRS PS1 - Preliminary results". Icarus. 261: 34–47. arXiv:1506.00762. Bibcode:2015Icar..261...34V. doi:10.1016/j.icarus.2015.08.007. Retrieved 15 March 2018.
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