Astronomy:5426 Sharp

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5426 Sharp
Discovery [1]
Discovered byC. Shoemaker
Discovery sitePalomar Obs.
Discovery date16 February 1985
Designations
(5426) Sharp
Named afterRobert P. Sharp
(American geomorphologist)[2]
1985 DD
Minor planet categorymain-belt · (inner) [1]
Hungaria [3][4]
Orbital characteristics [1]
Epoch 4 September 2017 (JD 2458000.5)
Uncertainty parameter 0
Observation arc31.94 yr (11,667 days)
|{{{apsis}}}|helion}}2.1828 AU
|{{{apsis}}}|helion}}1.7273 AU
1.9550 AU
Eccentricity0.1165
Orbital period2.73 yr (998 days)
Mean anomaly319.59°
Mean motion0° 21m 38.16s / day
Inclination23.795°
Longitude of ascending node88.178°
67.532°
Known satellites1[5][6] (suspected; P: 24.22 h)
Physical characteristics
Dimensions2.033±0.343 km[7][8]
3.85 km (calculated)[4]
Rotation period4.56±0.01 h[9]
4.5609±0.0001 h[5][lower-alpha 1]
Geometric albedo0.30 (assumed)[4]
1.000±0.000[7][8]
E [4]
Absolute magnitude (H)13.7[7] · 14.0[1][4] · 15.16±0.21[10]


5426 Sharp, provisional designation 1985 DD, is a bright Hungaria asteroid and suspected binary system from the inner regions of the asteroid belt, approximately 2–3 kilometers in diameter. It was discovered on 16 February 1985, by American astronomer Carolyn Shoemaker at Palomar Observatory, California, and named after American geologist Robert P. Sharp.[2][3]

Classification and orbit

Sharp is a bright E-type asteroid and a member of the Hungaria family, which form the innermost dense concentration of asteroids in the Solar System. It orbits the Sun in the inner main-belt at a distance of 1.7–2.2 AU once every 2 years and 9 months (998 days). Its orbit has an eccentricity of 0.12 and an inclination of 24° with respect to the ecliptic.[1] The body's observation arc begins with its official discovery observation at Palomar, as no precoveries were taken, and no prior identifications were made.[3]

Diameter and albedo

According to the surveys carried out by NASA's Wide-field Infrared Survey Explorer with its subsequent NEOWISE mission, Sharp measures 2.033 kilometers in diameter, and its surface has an outstandingly high albedo of 1.000.[7][8] The Collaborative Asteroid Lightcurve Link assumes an albedo of 0.30 – a compromise value between 0.4 and 0.2, corresponding to the Hungaria asteroids both as family and orbital group – and calculates a diameter of 3.85 kilometers with an absolute magnitude of 14.0.[4]

The high albedo derived from the WISE-observations indicate that Sharp belongs to the collisional Hungaria asteroids (rather than just its orbital group), which is thought to have originated from the same parent body that shattered into fragments in an ancient asteroid collision. The high albedo is due to the magnesium-rich mineral enstatite, which led to the E-type in the asteroid spectral type taxonomy.[5]

Suspected binary

A first rotational lightcurve of Sharp was obtained in November 2011, from photometric observations by American astronomer Brian Warner at his Palmer Divide Observatory (716) in Colorado ({{{1}}}).[9] Lightcurve analysis indicated the possibility that Sharp could be orbited by a minor-planet moon nearly every 24 hours.

In 2014/15, Sharp was re-examined by Brian Warner in a collaboration with astronomers Vladimir Benishek at Belgrade Astronomical Observatory, Serbia, and Andrea Ferrero at Bigmuskie Observatory in Italy (B88). The European collaboration was required because the satellite's orbital period was expected to be almost exactly an Earth day, and therefore synchronous with Earth, which would have made it impossible to obtain photometric data points covering the entire lightcurve from just one single location.[5]

The obtained lightcurves[lower-alpha 1] from the combined photometric observations gave a well-defined rotation period of 4.5609 hours, a brightness variation of 0.18 magnitude ({{{1}}}), and orbital period of 24.22 hours for the asteroid's moon. However, as no mutual occultation/eclipsing events were observed, the binary nature of Sharp remains unconfirmed.[5] The "Johnstonsarchive" estimates that the moon has a semi-major axis of 4.5 kilometers.[6] No diameter estimate for the moon was published, as a secondary-to-primary mean-diameter ratio could not be derived.

Naming

This minor planet was named in honor of American geomorphologist Robert P. Sharp (1911–2004), American professor of geology at Caltech, expert on glaciers, the movement of sand dunes and the geology of Mars. The Martian crater Robert Sharp and mountain Mount Sharp (now officially Aeolis Mons), were named in his honor. Mount Sharp rises from the middle of Gale Crater, which is explored by the Mars Curiosity rover since 2012.[2] The approved naming citation was published by the Minor Planet Center on 17 March 1995 (M.P.C. 24917).[11]

Notes

  1. ↑ 1.0 1.1 Three lightcurve plots of (5426) Sharp, obtained by Brian D. Warner in collaboration with Vladimir Benishek and Andrea Ferrero between December 2014 and January 2015[5]

References

  1. ↑ 1.0 1.1 1.2 1.3 1.4 "JPL Small-Body Database Browser: 5426 Sharp (1985 DD)". Jet Propulsion Laboratory. https://ssd.jpl.nasa.gov/sbdb.cgi?sstr=2005426. 
  2. ↑ 2.0 2.1 2.2 Schmadel, Lutz D. (2007). "(5426) Sharp". Dictionary of Minor Planet Names – (5426) Sharp. Springer Berlin Heidelberg. p. 464. doi:10.1007/978-3-540-29925-7_5208. ISBN 978-3-540-00238-3. 
  3. ↑ 3.0 3.1 3.2 "5426 Sharp (1985 DD)". Minor Planet Center. https://www.minorplanetcenter.net/db_search/show_object?object_id=5426. 
  4. ↑ 4.0 4.1 4.2 4.3 4.4 4.5 "LCDB Data for (5426) Sharp". Asteroid Lightcurve Database (LCDB). http://www.minorplanet.info/PHP/generateOneAsteroidInfo.php?AstInfo=5426%7CSharp. 
  5. ↑ 5.0 5.1 5.2 5.3 5.4 5.5 Warner, Brian D.; Benishek, Vladimir; Ferrero, Andrea (July 2015). "5426 Sharp: A Probable Hungaria Binary". The Minor Planet Bulletin 42 (3): 206–207. ISSN 1052-8091. Bibcode: 2015MPBu...42..206W. http://adsabs.harvard.edu/cgi-bin/bib_query?bibcode=2015MPBu...42..206W. Retrieved 30 March 2017. 
  6. ↑ 6.0 6.1 Johnston, Robert (23 June 2015). "(5426) Sharp". http://www.johnstonsarchive.net/astro/astmoons/am-05426.html. 
  7. ↑ 7.0 7.1 7.2 7.3 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. 
  8. ↑ 8.0 8.1 8.2 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. http://adsabs.harvard.edu/cgi-bin/bib_query?bibcode=2011ApJ...741...68M. Retrieved 30 March 2017. 
  9. ↑ 9.0 9.1 Warner, Brian D. (April 2012). "Asteroid Lightcurve Analysis at the Palmer Divide Observatory: 2011 September - December". The Minor Planet Bulletin 39 (2): 69–80. ISSN 1052-8091. Bibcode: 2012MPBu...39...69W. http://adsabs.harvard.edu/cgi-bin/bib_query?bibcode=2012MPBu...39...69W. Retrieved 30 March 2017. 
  10. ↑ 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. http://adsabs.harvard.edu/cgi-bin/bib_query?bibcode=2015Icar..261...34V. Retrieved 30 March 2017. 
  11. ↑ "MPC/MPO/MPS Archive". Minor Planet Center. https://www.minorplanetcenter.net/iau/ECS/MPCArchive/MPCArchive_TBL.html. 

External links



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