1146 Biarmia, provisional designation1929 JF, is a metallic backgroundasteroid from the outer regions of theasteroid belt, approximately 32 kilometers in diameter. It was discovered on 7 May 1929, by Russian astronomerGrigory Neujmin at theSimeiz Observatory on the Crimean peninsula.[17] The asteroid was named for theBjarmaland mentioned in Norse sagas.
Biarmia is not a member of any knownasteroid family. It orbits the Sun in theouter main-belt at a distance of 2.3–3.8 AU once every 5 years and 4 months (1,940 days). Its orbit has aneccentricity of 0.26 and aninclination of 17° with respect to theecliptic.[1]
The asteroid was first identified asA913 KA at Winchester Observatory (799) in June 1913. The body'sobservation arc begins with its official discovery observation at Simeiz.[17]
The best-rated rotationallightcurves ofBiarmia were obtained from photometric observations at the Etscorn Observatory (719), New Mexico, and at the S.O.S. Observatory (H39) in Minnesota, United States. Lightcurve analysis gave arotation period of 5.468 and 5.4700 hours with a brightness amplitude of 0.22 and 0.20magnitude, respectively (U=3/3).[11][12][a]
Other observations received a lower rating or have since been retracted.[b] Warner's period of 11.514 hours was later revised to 5.33 (U=2).[10][13]
TheCollaborative Asteroid Lightcurve Link adopts the results obtained by IRAS, that is, a stony albedo of 0.2190 and a diameter of 31.14 kilometers based on anabsolute magnitude of 9.80.[4]
^abLightcurve plot of 1146 Biarmia with a period of 5.47 hours. Brian D. Warner. Note by Warner: "Originally reported in MPB 27, 4-6 with P = 11.514 and A = 0.32. Reanalysis found revised period of P = 5.33, which disagrees with the 5.47 found by Durkee. The curve above is plotted to the Durkee period, which does give a better fit than with 5.33 h."
^abBehrend (2008) web: obs. date: 27 January 2008. Rotation period21.6 hours with a brightness amplitude of0.07 mag. Summary figures for (1146) Biarmia atCollaborative Asteroid Lightcurve Link (CALL). Lightcurve was removed fromwebsite by Raoul Behrend.
^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.
^abcMasiero, 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.
^abWarner, Brian D. (January 2011). "Upon Further Review: III. An Examination of Previous Lightcurve Analysis from the Palmer Divide Observatory".The Minor Planet Bulletin.38 (1):21–23.Bibcode:2011MPBu...38...21W.ISSN1052-8091.
^abKlinglesmith, Daniel A. III; Hanowell, Jesse; Warren, Curtis Alan (October 2014). "Lightcurves for Inversion Model Candidates".The Minor Planet Bulletin.41 (4):206–208.Bibcode:2014MPBu...41..206K.ISSN1052-8091.
^abDurkee, Russell I. (October 2009). "The Lightcurves of 1146 Biarmia and 5598 Carlmurray".The Minor Planet Bulletin.36 (4): 170.Bibcode:2009MPBu...36..170D.ISSN1052-8091.
^abWarner, B. (March 2000). "Asteroid Photometry at the Palmer Divide Observatory".The Minor Planet Bulletin.27:4–6.Bibcode:2000MPBu...27....4W.
