1144 Oda

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1144 Oda
Discovery [1]
Discovered by K. Reinmuth
Discovery site Heidelberg Obs.
Discovery date 28 January 1930
MPC designation (1144) Oda
Named after
A girl's name picked from a
popular German calendar[2]
1930 BJ · 1959 CJ
1967 EV
main-belt · (outer)
Orbital characteristics[1]
Epoch 4 September 2017 (JD 2458000.5)
Uncertainty parameter 0
Observation arc 87.27 yr (31,875 days)
Aphelion 4.1018 AU
Perihelion 3.3959 AU
3.7489 AU
Eccentricity 0.0942
7.26 yr (2,651 days)
0° 8m 8.88s / day
Inclination 9.7423°
Physical characteristics
Dimensions 56.347±0.194 km[4]
57.59±2.2 km[5]
57.65 km (derived)[3]
64.21±0.96 km[6]
14.4 h (dated)[7]
44.023±0.2530 h[8]
0.0583 (derived)[3]
Tholen = D[1][3] · X[9]
B–V = 0.706 [1]
U–B = 0.249 [1]
9.794±0.002 (R)[8] · 9.9[3] · 10.00[1][5][6] · 10.05±0.54[9]

1144 Oda, provisional designation 1930 BJ, is a dark Hildian asteroid from the outermost regions of the asteroid belt, approximately 57 kilometers in diameter. It was discovered on 28 January 1930, by German astronomer Karl Reinmuth at the Heidelberg-Königstuhl State Observatory.[10] The asteroid's name is a German female name, not related to the discoverer's contemporaries.[2]

Orbit and classification[edit]

Oda belongs to the dynamical Hilda group which is located in the outermost part of the main belt.[3] Asteroids in this group have semi-major axis between 3.7 and 4.2 AU and stay in a 3:2 resonance with the gas giant Jupiter. Oda, however, is a non-family background asteroid, i.e. not a member of the collisional Hilda family (001).[11]

It orbits the Sun in the outer main belt at a distance of 3.4–4.1 AU once every 7 years and 3 months (2,651 days). Its orbit has an eccentricity of 0.09 and an inclination of 10° with respect to the ecliptic.[1] The body's observation arc begins at Heidelberg, two months after its official discovery observation.[10]

Physical characteristics[edit]

In the Tholen classification, Oda is a dark and reddish D-type asteroid.[1] It has also been characterized as an X-type by PanSTARRS photometric survey.[9]

Rotation period[edit]

In May 2011, a rotational lightcurve of Oda was obtained from photometric observations in the R-band by astronomers at the Palomar Transient Factory in California. Lightcurve analysis gave a rotation period of 44.023 hours with a brightness variation of 0.41 magnitude (U=2).[8] A previously measured period of 14.4 is now considered incorrect (U=1).[7]

While not being a slow rotator, which have periods above 100 hours, Oda's spin rate is significantly longer than that of most other asteroids that have periods shorter than 20 hours.

Diameter and albedo[edit]

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, Oda measures between 56.347 and 64.21 kilometers in diameter and its surface has an albedo between 0.043 and 0.061.[4][5][6]

The Collaborative Asteroid Lightcurve Link derives an albedo of 0.0583 and a diameter of 57.65 kilometers based on an absolute magnitude of 9.9.[3]


This minor planet was named after a girl's name picked from the German popular calendar Der Lahrer hinkende Bote (de).

As with 913 Otila, Reinmuth selected names from this calendar due to his many asteroid discoveries that he had trouble thinking of proper names. These names are not related to the discoverer's contemporaries. The author of the Dictionary of Minor Planet Names learned about Reinmuth's source of inspiration from private communications with Dutch astronomer Ingrid van Houten-Groeneveld, who worked as a young astronomer at Heidelberg.[2]


  1. ^ a b c d e f g h "JPL Small-Body Database Browser: 1144 Oda (1930 BJ)" (2017-05-06 last obs.). Jet Propulsion Laboratory. Retrieved 9 September 2017. 
  2. ^ a b c Schmadel, Lutz D. (2007). Dictionary of Minor Planet Names – (1144) Oda. Springer Berlin Heidelberg. p. 97. ISBN 978-3-540-00238-3. Retrieved 9 September 2017. 
  3. ^ a b c d e f g "LCDB Data for (1144) Oda". Asteroid Lightcurve Database (LCDB). Retrieved 9 September 2017. 
  4. ^ a b c Grav, T.; Mainzer, A. K.; Bauer, J.; Masiero, J.; Spahr, T.; McMillan, R. S.; et al. (January 2012). "WISE/NEOWISE Observations of the Hilda Population: Preliminary Results". The Astrophysical Journal. 744 (2): 15. arXiv:1110.0283Freely accessible. Bibcode:2012ApJ...744..197G. doi:10.1088/0004-637X/744/2/197. Retrieved 9 September 2017. 
  5. ^ 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. Bibcode:2004PDSS...12.....T. Retrieved 9 September 2017. 
  6. ^ 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. Retrieved 9 September 2017. 
  7. ^ a b Behrend, Raoul. "Asteroids and comets rotation curves – (1144) Oda". Geneva Observatory. Retrieved 9 September 2017. 
  8. ^ a b c 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:1504.04041Freely accessible. Bibcode:2015AJ....150...75W. doi:10.1088/0004-6256/150/3/75. Retrieved 9 September 2017. 
  9. ^ a b c 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" (PDF). Icarus. 261: 34–47. arXiv:1506.00762Freely accessible. Bibcode:2015Icar..261...34V. doi:10.1016/j.icarus.2015.08.007. Retrieved 9 September 2017. 
  10. ^ a b "1144 Oda (1930 BJ)". Minor Planet Center. Retrieved 9 September 2017. 
  11. ^ "Small Bodies Data Ferret". Nesvorny HCM Asteroid Families V3.0. Retrieved 8 September 2017. 

External links[edit]