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1109 Tata

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1109 Tata
Discovery[1]
Discovered byK. Reinmuth
Discovery siteHeidelberg Obs.
Discovery date5 February 1929
Designations
(1109) Tata
Named after
unknown[2]
1929 CU · 1925 QE
1964 HA
main-belt[1] · (outer)[3][4]
Hygiea[5]
Orbital characteristics[3]
Epoch 23 March 2018 (JD 2458200.5)
Uncertainty parameter 0
Observation arc88.95 yr (32,489 d)
Aphelion3.5443 AU
Perihelion2.9085 AU
3.2264 AU
Eccentricity0.0985
5.80 yr (2,117 d)
96.944°
0° 10m 12.36s / day
Inclination4.1199°
268.08°
359.39°
Physical characteristics
61.817±0.265 km[6]
62.39±0.36 km[7]
63.2±12.6 km[8]
64±6 km[9]
65.677±0.810 km[10]
66.49±1.32 km[11]
66.53±1.4 km[12]
69.640±22.05 km[13]
74.94±22.96 km[14]
8.277±0.002 h[15]
0.0378±0.002[12]
0.038±0.002[11]
0.0387±0.0080[10]
0.04±0.01[9]
0.04±0.02[8][14]
0.043±0.010[7]
0.044±0.005[6]
0.0485±0.0416[13]
Tholen = FC[3][4] · P[10]
B–V = 0.604[3]
9.89[13] · 9.89±0.27[16]
10.06[3][4][7][8][9][10][11][12][14]

1109 Tata, provisional designation 1929 CU, is a dark Hygiean asteroid from the outer regions of the asteroid belt, approximately 69 kilometers (43 miles) in diameter. It was discovered on 5 February 1929, by German astronomer Karl Reinmuth at the Heidelberg-Königstuhl State Observatory in Germany.[1] The meaning of the asteroids's name is unknown.[2]

Orbit and classification

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Tata is a member of the Hygiea family (601),[5] a very large family of carbonaceous outer-belt asteroids. The family's parent body and namesake is the main belt's fourth-largest asteroid, 10 Hygiea.[17] It orbits the Sun in the outer asteroid belt at a distance of 2.9–3.5 AU once every 5 years and 10 months (2,117 days; semi-major axis of 3.23 AU). Its orbit has an eccentricity of 0.10 and an inclination of 4° with respect to the ecliptic.[3]

The asteroid was first observed as 1925 QE at Simeiz Observatory in March 1925. The body's observation arc begins at Heidelberg in March 1929, one month after its official discovery observation.[1]

Physical characteristics

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In the Tholen classification, Tata has an ambiguous spectral type, closest to the rare F-types and somewhat similar to the common carbonaceous C-type asteroids.[3][4] It has also been characterized as a primitive P-type asteroid by the space-based Wide-field Infrared Survey Explorer (WISE).[10]

Rotation period

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In July 2005, a rotational lightcurve of Tata was obtained from photometric observations by French amateur astronomer Laurent Bernasconi. Lightcurve analysis gave a rotation period of 8.277 hours with a low brightness amplitude of 0.06 magnitude (U=2), indicative for a spherical shape. The astronomer also reported that several other period solution could be possible.[15]

Diameter and albedo

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According to the surveys carried out by the Infrared Astronomical Satellite IRAS, the Japanese Akari satellite and the NEOWISE mission of NASA's WISE telescope, Tata measures between 61.817 and 74.94 kilometers in diameter and its surface has an albedo between 0.0378 and 0.0485.[6][7][8][9][10][11][12][13][14]

The Collaborative Asteroid Lightcurve Link adopts the results obtained by IRAS, that is, an albedo of 0.0378 and a diameter of 66.53 kilometers based on an absolute magnitude of 10.06.[4]

Naming

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Any reference of this minor planet's name to a person or occurrence is unknown.[2]

Unknown meaning

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Among the many thousands of named minor planets, Tata is one of 120 asteroids, for which no official naming citation has been published. All of these asteroids have low numbers between 164 Eva and 1514 Ricouxa and were discovered between 1876 and the 1930s, predominantly by astronomers Auguste Charlois, Johann Palisa, Max Wolf and Karl Reinmuth.[18]

References

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  1. ^ a b c d "1109 Tata (1929 CU)". Minor Planet Center. Retrieved 6 March 2018.
  2. ^ a b c Schmadel, Lutz D. (2007). "(1109) Tata". Dictionary of Minor Planet Names. Springer Berlin Heidelberg. p. 94. doi:10.1007/978-3-540-29925-7_1110. ISBN 978-3-540-00238-3.
  3. ^ a b c d e f g "JPL Small-Body Database Browser: 1109 Tata (1929 CU)" (2018-01-18 last obs.). Jet Propulsion Laboratory. Retrieved 6 March 2018.
  4. ^ a b c d e "LCDB Data for (1109) Tata". Asteroid Lightcurve Database (LCDB). Retrieved 6 March 2018.
  5. ^ a b "Asteroid 1109 Tata – Nesvorny HCM Asteroid Families V3.0". Small Bodies Data Ferret. Retrieved 26 October 2019.
  6. ^ 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.
  7. ^ a b c d 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 6 March 2018.
  8. ^ a b c d Alí-Lagoa, V.; Licandro, J.; Gil-Hutton, R.; Cañ; ada-Assandri, M.; Delbo', M.; et al. (June 2016). "Differences between the Pallas collisional family and similarly sized B-type asteroids". Astronomy and Astrophysics. 591: 11. Bibcode:2016A&A...591A..14A. doi:10.1051/0004-6361/201527660. hdl:11336/63614.
  9. ^ a b c d Alí-Lagoa, V.; de León, J.; Licandro, J.; Delbó, M.; Campins, H.; Pinilla-Alonso, N.; et al. (June 2013). "Physical properties of B-type asteroids from WISE data". Astronomy and Astrophysics. 554: 16. arXiv:1303.5487. Bibcode:2013A&A...554A..71A. doi:10.1051/0004-6361/201220680. Retrieved 6 March 2018.
  10. ^ a b c d e f 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.
  11. ^ 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)
  12. ^ a b c d 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.
  13. ^ a b c d Masiero, Joseph R.; Nugent, C.; Mainzer, A. K.; Wright, E. L.; Bauer, J. M.; Cutri, R. M.; et al. (October 2017). "NEOWISE Reactivation Mission Year Three: Asteroid Diameters and Albedos". The Astronomical Journal. 154 (4): 10. arXiv:1708.09504. Bibcode:2017AJ....154..168M. doi:10.3847/1538-3881/aa89ec.
  14. ^ a b c d Nugent, C. R.; Mainzer, A.; Masiero, J.; Bauer, J.; Cutri, R. M.; Grav, T.; et al. (December 2015). "NEOWISE Reactivation Mission Year One: Preliminary Asteroid Diameters and Albedos". The Astrophysical Journal. 814 (2): 13. arXiv:1509.02522. Bibcode:2015ApJ...814..117N. doi:10.1088/0004-637X/814/2/117. Retrieved 6 March 2018.
  15. ^ a b Behrend, Raoul. "Asteroids and comets rotation curves – (1109) Tata". Geneva Observatory. Retrieved 6 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 6 March 2018.
  17. ^ Nesvorný, D.; Broz, M.; Carruba, V. (December 2014). "Identification and Dynamical Properties of Asteroid Families". Asteroids IV. pp. 297–321. arXiv:1502.01628. Bibcode:2015aste.book..297N. doi:10.2458/azu_uapress_9780816532131-ch016. ISBN 9780816532131.
  18. ^ Schmadel, Lutz D. (2007). "Appendix 11 – Minor Planet Names with Unknown Meaning". Dictionary of Minor Planet Names – Fifth Revised and Enlarged revision. Springer Berlin Heidelberg. pp. 927–929. ISBN 978-3-540-00238-3.
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