166 Rhodope is a dark backgroundasteroid from the central region of theasteroid belt, approximately 55 kilometers in diameter. It was discovered on 15 August 1876, by German–American astronomerChristian Peters at theLitchfield Observatory in Clinton, New York, United States.[17] The asteroid was named afterQueen Rhodope from Greek mythology.[3]
Rhodope orbits the Sun in thecentral asteroid belt at a distance of 2.1–3.3 AU once every 4 years and 5 months (1,607 days). Its orbit has aneccentricity of 0.21 and aninclination of 12° with respect to theecliptic.[1] The body'sobservation arc begins with the first recorded observation by theMPC atVienna Observatory on 10 September 1885, or more than 9 years after its official discovery observation at Clinton.[17]
Two well-defined rotationallightcurves ofRhodope were obtained from photometric observations by French astronomer Matthieu Conjat and by an anonymous observer of theCollaborative Asteroid Lightcurve Link (CALL). Lightcurve analysis gave a consolidatedrotation period of 4.715 hours with a brightness variation of 0.35 to 0.36magnitude (U=3/3).[5][14][a] The result supersedes a period of 7.87 hours measured by Alan Harris in the early 1980s (U=1).[15]
In 2013, the asteroid's lightcurve was also modeled from combined dense and sparsephotometry. It gave a concurring sidereal period of 4.714793 hours. The modelling also determined two spin axis of (345.0°, −22.0°) and (173.0°, −3.0°) inecliptic coordinates (λ, β).[13]
According to the surveys carried out by the JapaneseAkari satellite and theNEOWISE mission of NASA's WISE telescope,Rhodope measures between 39.04 and 65.29 kilometers in diameter and its surface has analbedo between 0.046 and 0.10.[6][7][8][9][10][11][12]
CALL adoptsPetr Pravec's revised WISE-data, that is, an albedo of 0.0747 and a diameter of 54.56 kilometers based on anabsolute magnitude of 9.75.[5][10]
^abcdUsui, 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)
^abcdePravec, 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.
^abcdMasiero, 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.S2CID46350317.
^abHanus, J.; Durech, J.; Broz, M.; Marciniak, A.; Warner, B. D.; Pilcher, F.; et al. (March 2013). "Asteroids' physical models from combined dense and sparse photometry and scaling of the YORP effect by the observed obliquity distribution".Astronomy and Astrophysics.551: 16.arXiv:1301.6943.Bibcode:2013A&A...551A..67H.doi:10.1051/0004-6361/201220701.S2CID118627434.