Astronomy:5477 Holmes

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5477 Holmes
Discovery [1]
Discovered byE. F. Helin
Discovery sitePalomar Obs.
Discovery date27 October 1989
Designations
(5477) Holmes
Named afterRobert Holmes [1]
(American astronomer)
1989 UH2
Minor planet categorymain-belt · (inner) [2]
Hungaria [1][3][4]
Orbital characteristics [2]
Epoch 23 March 2018 (JD 2458200.5)
Uncertainty parameter 0
Observation arc27.60 yr (10,082 d)
|{{{apsis}}}|helion}}2.0613 AU
|{{{apsis}}}|helion}}1.7732 AU
1.9172 AU
Eccentricity0.0751
Orbital period2.65 yr (970 d)
Mean anomaly295.23°
Mean motion0° 22m 16.68s / day
Inclination22.552°
Longitude of ascending node49.112°
290.30°
Known satellites1 (D: 1.09 km P: 24.4 h)[3][5][6]
Physical characteristics
Mean diameter2.95±0.13 km (derived)[5]
3.147±0.137 km[7][8]
3.21 km (taken)[3]
3.215 km[9]
Rotation period2.9932±0.0002 h[10][lower-alpha 1]
2.9940±0.0002 h[11]
2.99401±0.00007 h[12]
2.99408±0.00007 h[13]
2.9943±0.0002 h[6]
Geometric albedo0.2849[9]
0.310±0.038[7][8]
E (assumed)[3]
Absolute magnitude (H)13.99±0.03 (R)[12]
14.0[2]
14.26±0.54[14]
14.4[8][13]
14.445[3][9]


5477 Holmes, provisional designation 1989 UH2, is a Hungaria asteroid and binary system from the innermost regions of the asteroid belt, approximately 3 kilometers (2 miles) in diameter. It was discovered on 27 October 1989, by American astronomer Eleanor Helin at the Palomar Observatory in California.[1] The presumed E-type asteroid is likely spherical in shape and has a short rotation period of 2.99 hours.[3] It was named for American amateur astronomer Robert Holmes.[1] The discovery of its 1-kilometer-sized minor-planet moon was announced in November 2005.[5][6]

Orbit and classification

Holmes is a core member of the Hungaria family (003),[4] a large family of bright asteroids that forms the innermost dense concentration of asteroids in the Solar System, as the Mars-crosser and near-Earth populations are much more sparse. The family is part of the larger dynamical group with the same name.[1][3] It orbits the Sun in the innermost asteroid belt at a distance of 1.8–2.1 AU once every 2 years and 8 months (970 days; semi-major axis of 1.92 AU). Its orbit has an eccentricity of 0.08 and an inclination of 23° with respect to the ecliptic.[2] The body's observation arc begins with its official discovery observation at Palomar in October 1989.[1]

Physical characteristics

Holmes is an assumed E-type asteroid,[3] which agrees with the overall spectral type for members of the Hungaria family.[15]:23

Rotation period

Since 2005, several rotational lightcurves of Holmes have been obtained from photometric observations by Brian Warner and Petr Pravec in collaboration with other astronomers.[6][10][11][12][13][lower-alpha 1] Analysis of the best-rated lightcurve gave a well-defined rotation period of 2.9940 hours with a consolidated brightness amplitude between 0.10 and 0.12 magnitude, which indicates that the body has a nearly spherical shape ({{{1}}}).[3][11] The asteroid's short period is near that of a fast rotator.

Diameter and albedo

According to the survey carried out by the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer (WISE), Holmes measures 3.147 kilometers in diameter and its surface has an albedo of 0.31,[7][8] while the Collaborative Asteroid Lightcurve Link adopts Petr Pravec's revised WISE-data, that is, an albedo of 0.2849 and a diameter of 3.21 kilometers based on an absolute magnitude of 14.445.[3][9] Johnston's Archive derives a diameter of 2.95 and 3.15 kilometers for the primary only and for the combined system, respectively.[5]

Satellite

The photometric observations obtained by Brian Warner and collaborators during 2–12 November 2005,[13] revealed that Holmes is a synchronous binary asteroid with a minor-planet moon orbiting it every 24.4 hours at an estimated average distance of 6.7 km. The discovery was announced immediately on 15 November 2005.[6] The mutual occultation events indicated the presence of a satellite 37% the size of its primary, which translates into an estimated diameter of 1.09–1.19 kilometers depending on the underlying size estimate of the primary.[3][5]

Naming

This minor planet was named after American amateur astronomer Robert E. Holmes Jr (born 1956), who directs the Astronomical Research Observatory (H21) in Westfield, Illinois.[1] The official naming citation was suggested by Sergio Foglia and published by the Minor Planet Center on 18 February 2011 (M.P.C. 73983).[16]

Notes

  1. ↑ 1.0 1.1 Lightcurve plot of 5477 Holmes, Palmer Divide Observatory, Brian D. Warner (2012). Rotation period 2.9932±0.0002 hours with a brightness amplitude of 0.10±0.01 mag. The second plot for the orbital period of the satellite gives a period of 24.37±0.01 hours. Quality code is 3. Summary figures at the LCDB.

References

  1. ↑ 1.0 1.1 1.2 1.3 1.4 1.5 1.6 1.7 "5477 Holmes (1989 UH2)". Minor Planet Center. https://www.minorplanetcenter.net/db_search/show_object?object_id=5477. 
  2. ↑ 2.0 2.1 2.2 2.3 "JPL Small-Body Database Browser: 5477 Holmes (1989 UH2)". Jet Propulsion Laboratory. https://ssd.jpl.nasa.gov/sbdb.cgi?sstr=2005477. 
  3. ↑ 3.00 3.01 3.02 3.03 3.04 3.05 3.06 3.07 3.08 3.09 3.10 "LCDB Data for (5477) Holmes". Asteroid Lightcurve Database (LCDB). http://www.minorplanet.info/PHP/generateOneAsteroidInfo.php?AstInfo=5477%7CHolmes. 
  4. ↑ 4.0 4.1 "Asteroid 5477 Holmes". Small Bodies Data Ferret. https://sbntools.psi.edu/ferret/SimpleSearch/results.action?targetName=5477+Holmes. 
  5. ↑ 5.0 5.1 5.2 5.3 5.4 Johnston, Wm. Robert (21 September 2014). "Asteroids with Satellites Database – (5477) Holmes". Johnston's Archive. http://www.johnstonsarchive.net/astro/astmoons/am-05477.html. 
  6. ↑ 6.0 6.1 6.2 6.3 6.4 Warner, B. D.; Pravec, P.; Kusnirak, P.; Cooney, W.; Gross, J.; Terrell, D. et al. (November 2005). "CBET #288 – (5477) 1989 UH_2". Central Bureau Electronic Telegrams 288 (288): 1. Bibcode: 2005CBET..288....1W. http://www.cbat.eps.harvard.edu/iau/cbet/000200/CBET000288.txt. Retrieved 17 May 2018. 
  7. ↑ 7.0 7.1 7.2 Masiero, Joseph R.; Mainzer, A. K.; Grav, T.; Bauer, J. M.; Cutri, R. M.; Dailey, J. et al. (November 2011). "Main Belt Asteroids with WISE/NEOWISE. I. Preliminary Albedos and Diameters". The Astrophysical Journal 741 (2): 20. doi:10.1088/0004-637X/741/2/68. Bibcode: 2011ApJ...741...68M. 
  8. ↑ 8.0 8.1 8.2 8.3 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. doi:10.1088/0004-637X/741/2/90. Bibcode: 2011ApJ...741...90M.  (catalog)
  9. ↑ 9.0 9.1 9.2 9.3 Pravec, 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. doi:10.1016/j.icarus.2012.07.026. Bibcode: 2012Icar..221..365P. 
  10. ↑ 10.0 10.1 Warner, Brian D.; Stephens, Robert D.; Coley Daniel (October 2012). "Lightcurve for the Hungaria Binary 5477 Holmes". The Minor Planet Bulletin 39 (4): 230–231. ISSN 1052-8091. Bibcode: 2012MPBu...39..230W. 
  11. ↑ 11.0 11.1 11.2 Pravec, P.; Scheirich, P.; Kusnirák, P.; Hornoch, K.; Galád, A.; Naidu, S. P. et al. (March 2016). "Binary asteroid population. 3. Secondary rotations and elongations". Icarus 267: 267–295. doi:10.1016/j.icarus.2015.12.019. Bibcode: 2016Icar..267..267P. 
  12. ↑ 12.0 12.1 12.2 Pravec, P.; Scheirich, P.; Vokrouhlický, D.; Harris, A. W.; Kusnirák, P.; Hornoch, K. et al. (March 2012). "Binary asteroid population. 2. Anisotropic distribution of orbit poles of small, inner main-belt binaries". Icarus 218 (1): 125–143. doi:10.1016/j.icarus.2011.11.026. Bibcode: 2012Icar..218..125P. 
  13. ↑ 13.0 13.1 13.2 13.3 Warner, Brian D.; Pravec, Petr; Kusnirak, Peter; Harris, Alan W.; Cooney, Walter R. Jr.; Gross, John et al. (April 2011). "Lightcurves from the Initial Discovery of Four Hungaria Binary Asteroids". The Minor Planet Bulletin 38 (2): 107–109. ISSN 1052-8091. Bibcode: 2011MPBu...38..107W. 
  14. ↑ 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. doi:10.1016/j.icarus.2015.08.007. Bibcode: 2015Icar..261...34V. 
  15. ↑ Nesvorný, D.; Broz, M.; Carruba, V. (December 2014). "Identification and Dynamical Properties of Asteroid Families". Asteroids IV. pp. 297–321. doi:10.2458/azu_uapress_9780816532131-ch016. ISBN 9780816532131. Bibcode: 2015aste.book..297N. 
  16. ↑ "MPC/MPO/MPS Archive". Minor Planet Center. https://www.minorplanetcenter.net/iau/ECS/MPCArchive/MPCArchive_TBL.html. 

External links



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