Wikipedia

1088 Mitaka

1088 Mitaka (prov. designation: 1927 WA) is a bright background asteroid from the inner regions of the asteroid belt. It was discovered on 17 November 1927, by Japanese astronomer Okuro Oikawa at the old Tokyo Astronomical Observatory in Japan.[1] The stony S-type asteroid has a notably short rotation period of 3.0 hours and measures approximately 15 kilometers (9.3 miles) in diameter. It was named after the Japanese village of Mitaka.[2]

1088 Mitaka
Modelled shape of Mitaka from its lightcurve
Discovery[1]
Discovered byO. Oikawa
Discovery siteTokyo Astronomical Obs.
Discovery date17 November 1927
Designations
(1088) Mitaka
Named after
Mitaka[2] (Japanese village)
1927 WA · 1942 FR
1953 VW3 · 1971 BE
A917 RA
Orbital characteristics[3]
Epoch 4 September 2017 (JD 2458000.5)
Uncertainty parameter 0
Observation arc88.22 yr (32,224 days)
Aphelion2.6328 AU
Perihelion1.7722 AU
2.2025 AU
Eccentricity0.1954
3.27 yr (1,194 days)
200.92°
0° 18m 5.4s / day
Inclination7.6514°
54.495°
319.50°
Physical characteristics
11.33±2.51 km[6]
13.35±0.75 km[7]
15.137±0.131 km[8]
15.957±0.030 km[9]
16.016 km[10]
16.02 km (taken)[11]
3.027±0.003 h[12]
3.0353±0.0005 h[13]
3.035377 h[14]
3.035378±0.000005 h[15]
3.0354±0.0002 h[16]
3.0361±0.0007 h[16]
3.049±0.005 h[17]
  • (115.0°, 46.0°) (λ1/β1)[5]
  • (278.0°, −72.0°) (λ2/β2)[5]
0.1549[10]
0.1588±0.0204[9]
0.173±0.025[8]
0.276±0.034[7]
0.37±0.16[6]
11.39[3][7] · 11.55[6] · 11.62[11][9] · 11.62±0.08[10][17]

Orbit and classification

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Mitaka is a non-family asteroid of the main belt's background population when applying the hierarchical clustering method to its proper orbital elements.[4][5] 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 (1,194 days). Its orbit has an eccentricity of 0.20 and an inclination of 8° with respect to the ecliptic.[3] The asteroid was first observed as A917 RA at the Simeiz Observatory on 11 September 1917. The body's observation arc begins at Tokyo in December 1927, one month after its official discovery observation.[1]

Naming

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This minor planet was named after the Japanese village of Mitaka, where the discovering Tokyo Astronomical Observatory was located. Nowadays the city of Mitaka hosts the headquarters of the National Astronomical Observatory of Japan with the Tokyo Photoelectric Meridian Circle, public relation and data centers, and several telescopes. The official naming citation was mentioned in The Names of the Minor Planets by Paul Herget in 1955 (H 103).[2]

Physical characteristics

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Mitaka is a common, stony S-type asteroid in both the Tholen and Bus–Binzel SMASS classification.[3][11]

Rotation period and poles

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Several rotational lightcurves of Mitaka have been obtained from photometric observations since 1989.[12][13][16][17] Analysis of the best rated lightcurve by French amateur astronomer Pierre Antonini gave a rotation period of 3.0361 hours with a consolidated brightness variation of 0.23 to 0.62 magnitude (U=3).[11][16]

In 2009 and 2011, modelling of Mitaka's lightcurve using photometric data from the US Naval Observatory, the Uppsala Asteroid Photometric Catalogue (UAPC), the Palmer Divide Observatory's archive, the Palomar Transient Factory survey, and from individual observers, gave a concurring rotation period of 3.035377 and 3.035378 hours.[14][15] The modeled lightcurves also gave a spin axis of (115.0°, 46.0°) and (278.0°, −72.0°),[14] as well as (280.0°, −71.0°) in ecliptic coordinates (λ, β).[15]

Diameter and albedo

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According to the surveys carried out by the Japanese Akari satellite and the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer, Mitaka measures between 11.33 and 16.016 kilometers in diameter and its surface has an albedo between 0.1549 and 0.37.[6][7][8][9][10] The Collaborative Asteroid Lightcurve Link adopts Petr Pravec's revised WISE results with an albedo of 0.1549 and takes a diameter of 16.02 kilometers based on an absolute magnitude of 11.62.[11]

References

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  1. ^ a b c d "1088 Mitaka (1927 WA)". Minor Planet Center. Retrieved 27 September 2017.
  2. ^ a b c Schmadel, Lutz D. (2007). "(1088) Mitaka". Dictionary of Minor Planet Names – (1088) Mitaka. Springer Berlin Heidelberg. p. 93. doi:10.1007/978-3-540-29925-7_1089. ISBN 978-3-540-00238-3.
  3. ^ a b c d e f g h i "JPL Small-Body Database Browser: 1088 Mitaka (1927 WA)" (2017-07-05 last obs.). Jet Propulsion Laboratory. Retrieved 27 September 2017.
  4. ^ a b "Asteroid 1088 Mitaka – Proper Elements". AstDyS-2, Asteroids – Dynamic Site. Retrieved 13 March 2020.
  5. ^ a b c d "Asteroid 1088 Mitaka". Small Bodies Data Ferret. Retrieved 13 March 2020.
  6. ^ a b c d Nugent, C. R.; Mainzer, A.; Bauer, J.; Cutri, R. M.; Kramer, E. A.; Grav, T.; et al. (September 2016). "NEOWISE Reactivation Mission Year Two: Asteroid Diameters and Albedos". The Astronomical Journal. 152 (3): 12. arXiv:1606.08923. Bibcode:2016AJ....152...63N. doi:10.3847/0004-6256/152/3/63.
  7. ^ a b c d 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. (online, AcuA catalog p. 153)
  8. ^ a b c 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. S2CID 119293330. Retrieved 27 September 2017.
  9. ^ a b c d Mainzer, A.; Grav, T.; Masiero, J.; Hand, E.; Bauer, J.; Tholen, D.; et al. (November 2011). "NEOWISE Studies of Spectrophotometrically Classified Asteroids: Preliminary Results". The Astrophysical Journal. 741 (2): 25. arXiv:1109.6407. Bibcode:2011ApJ...741...90M. doi:10.1088/0004-637X/741/2/90. S2CID 35447010.
  10. ^ a b c d Pravec, Petr; Harris, Alan W.; Kusnirák, Peter; Galád, Adrián; Hornoch, Kamil (September 2012). "Absolute magnitudes of asteroids and a revision of asteroid albedo estimates from WISE thermal observations". Icarus. 221 (1): 365–387. Bibcode:2012Icar..221..365P. doi:10.1016/j.icarus.2012.07.026. Retrieved 27 September 2017.
  11. ^ a b c d e "LCDB Data for (1088) Mitaka". Asteroid Lightcurve Database (LCDB). Retrieved 27 September 2017.
  12. ^ a b Macias, Amadeo Aznar (January 2015). "Asteroid Lightcurve Analysis at Isaac Aznar Observatory Aras De Los Olmos, Valencia, Spain". The Minor Planet Bulletin. 42 (1): 4–6. Bibcode:2015MPBu...42....4M. ISSN 1052-8091. Retrieved 27 September 2017.
  13. ^ a b Kryszczynska, A.; Colas, F.; Polinska, M.; Hirsch, R.; Ivanova, V.; Apostolovska, G.; et al. (October 2012). "Do Slivan states exist in the Flora family?. I. Photometric survey of the Flora region". Astronomy and Astrophysics. 546: 51. Bibcode:2012A&A...546A..72K. doi:10.1051/0004-6361/201219199.
  14. ^ a b c Durech, J.; Kaasalainen, M.; Warner, B. D.; Fauerbach, M.; Marks, S. A.; Fauvaud, S.; et al. (January 2009). "Asteroid models from combined sparse and dense photometric data" (PDF). Astronomy and Astrophysics. 493 (1): 291–297. Bibcode:2009A&A...493..291D. doi:10.1051/0004-6361:200810393. Retrieved 24 August 2017.
  15. ^ a b c 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 27 September 2017.
  16. ^ a b c d Behrend, Raoul. "Asteroids and comets rotation curves – (1088) Mitaka". Geneva Observatory. Retrieved 27 September 2017.
  17. ^ a b c Wisniewski, W. Z.; Michalowski, T. M.; Harris, A. W.; McMillan, R. S. (March 1995). "Photoelectric Observations of 125 Asteroids". Abstracts of the Lunar and Planetary Science Conference. 26: 1511. Bibcode:1995LPI....26.1511W. Retrieved 27 September 2017.
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