1939 Loretta

From Wikipedia, the free encyclopedia

Jump to: navigation, search
1939 Loretta
Discovery [1]
Discovered by C. Kowal
Discovery site Palomar Obs.
Discovery date 17 October 1974
Designations
MPC designation 1939 Loretta
Named after
Loretta Kowal
(daughter of discoverer)[2]
1974 UC · 1934 JE
1934 LQ · 1939 EH
1939 GP · 1950 DT
1950 ES · 1951 MF
1955 CA · 1969 TE5
1975 TZ5 · 1975 XW
main-belt · Themistian[3]
Orbital characteristics[1]
Epoch 16 February 2017 (JD 2457800.5)
Uncertainty parameter 0
Observation arc 66.32 yr (24,224 days)
Aphelion 3.5190 AU
Perihelion 2.7291 AU
3.1241 AU
Eccentricity 0.1264
5.52 yr (2,017 days)
349.21°
0° 10m 42.6s / day
Inclination 0.9062°
40.480°
189.39°
Physical characteristics
Dimensions 26.34±0.46 km[4]
29.08±0.51 km[5]
29.83 km (derived)[3]
30.243±0.335 km[6]
30.365±0.351[7]
25 h[8]
0.0721 (derived)[3]
0.092±0.013[7]
0.0927±0.0089[6]
0.101±0.020[4]
0.103±0.004[5]
C[3]
10.8[5][6] · 11.0[4] · 11.1[1][3]

1939 Loretta, provisional designation 1974 UC, is a carbonaceous Themistian asteroid from the outer region of the asteroid belt, approximately 30 kilometers in diameter. It was discovered on 17 October 1974, by American astronomer Charles T. Kowal at Palomar Observatory in California, United States.[9]

The C-type asteroid is a member of the Themis family, a dynamical family of outer-belt asteroids with nearly coplanar ecliptical orbits.[3] It orbits the Sun at a distance of 2.7–3.5 AU once every 5 years and 6 months (2,017 days). Its orbit has an eccentricity of 0.13 and an inclination of 1° with respect to the ecliptic.[1] First identified as 1934 JE at the South African Johannesburg Observatory, Loretta's first used observation was made at the Finnish Turku Observatory in 1939, extending the body's observation arc by 35 years prior to its discovery.[9]

According to the surveys carried out by the Japanese Akari satellite and NASA's Wide-field Infrared Survey Explorer with its subsequent NEOWISE mission, Loretta measures between 26.3 and 30.4 kilometers in diameter, and its surface has an albedo between 0.092 and 0.101.[4][5][6][7] The Collaborative Asteroid Lightcurve Link derives an albedo of 0.072 and a diameter of 29.8 kilometers based on an absolute magnitude of 11.1.[3]

A fragmentary rotational light-curve of Loretta was obtained from photometric observations made by French amateur astronomer Pierre Antonini in March 2011. It gave an approxmiate rotation period of 25 hours with a brightness variation of 0.12 magnitude (U=1).[8]

The minor planet was named by the discoverer after his daughter, Loretta Kowal.[2] Naming citation was published before November 1977 (M.P.C. 3828).[10]

References[edit]

  1. ^ a b c d "JPL Small-Body Database Browser: 1939 Loretta (1974 UC)" (2016-06-16 last obs.). Jet Propulsion Laboratory. Retrieved 9 December 2016. 
  2. ^ a b Schmadel, Lutz D. (2007). Dictionary of Minor Planet Names – (1939) Loretta. Springer Berlin Heidelberg. p. 155. ISBN 978-3-540-00238-3. Retrieved 9 December 2016. 
  3. ^ a b c d e f g "LCDB Data for (1939) Loretta". Asteroid Lightcurve Database (LCDB). Retrieved 9 December 2016. 
  4. ^ 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:1209.5794Freely accessible. Bibcode:2012ApJ...759L...8M. doi:10.1088/2041-8205/759/1/L8. Retrieved 9 December 2016. 
  5. ^ 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" (PDF). Publications of the Astronomical Society of Japan. 63 (5): 1117–1138. Bibcode:2011PASJ...63.1117U. doi:10.1093/pasj/63.5.1117. Retrieved 9 December 2016. 
  6. ^ 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" (PDF). The Astrophysical Journal. 741 (2): 25. arXiv:1109.6407Freely accessible. Bibcode:2011ApJ...741...90M. doi:10.1088/0004-637X/741/2/90. Retrieved 9 December 2016. 
  7. ^ 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:1406.6645Freely accessible. Bibcode:2014ApJ...791..121M. doi:10.1088/0004-637X/791/2/121. Retrieved 9 December 2016. 
  8. ^ a b Behrend, Raoul. "Asteroids and comets rotation curves – (1939) Loretta". Geneva Observatory. Retrieved 9 December 2016. 
  9. ^ a b "1939 Loretta (1974 UC)". Minor Planet Center. Retrieved 9 December 2016. 
  10. ^ "MPC/MPO/MPS Archive". Minor Planet Center. Retrieved 9 December 2016. 

External links[edit]