9921 Rubincam

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9921 Rubincam
AnimatedOrbitOf99211981EO18.gif
Orbit of Rubincam (blue), inner planets and Jupiter (outermost)
Discovery [1]
Discovered by S. J. Bus
Discovery site Siding Spring Obs.
Discovery date 2 March 1981
Designations
MPC designation (9921) Rubincam
Named after
David Rubincam
(American geophysicist)[2]
1981 EO18
main-belt · (inner)[3]
Orbital characteristics[1]
Epoch 4 September 2017 (JD 2458000.5)
Uncertainty parameter 0
Observation arc 63.45 yr (23,175 days)
Aphelion|Aphelion 2.5174 AU
Perihelion|Perihelion 2.2352 AU
2.3763 AU
Eccentricity 0.0594
3.66 yr (1,338 days)
91.234°
0° 16m 8.76s / day
Inclination 2.4008°
331.39°
89.205°
Physical characteristics
Dimensions 4.10 km (calculated)[3]
4.250±0.094 km[4][5]
8.01±0.03 h[6]
8.014±0.0017 h[7]
0.20 (assumed)[3]
0.204±0.035[4][5]
S[3]
14.2[4] · 14.276±0.001 (R)[7] · 14.3[1][3]

9921 Rubincam, provisional designation 1981 EO18, is a stony asteroid from the inner regions of the asteroid belt, approximately 4 kilometers in diameter. It was discovered on 2 March 1981, by American astronomer Schelte Bus at the Siding Spring Observatory in Australia, and later named after American geophysicist David Rubincam.[2]

Orbit and classification[edit]

Rubincam is a stony S-type asteroid that orbits the Sun in the inner main-belt at a distance of 2.2–2.5 AU once every 3 years and 8 months (1,338 days). Its orbit has an eccentricity of 0.06 and an inclination of 2° with respect to the ecliptic.[1] A first precovery was taken at Palomar Observatory in 1953, extending the body's observation arc by 28 years prior to its official discovery at Siding Spring.[2]

Physical characteristics[edit]

Lightcurves[edit]

In February 2010, two rotational lightcurves of Rubincam were obtained from photometric observations at the Palomar Transient Factory in California. Lightcurve analysis gave a rotation period of 8.01 and 8.014 hours with a brightness amplitude of 0.33 and 0.31 in magnitude, respectively (U=3-/2).[6][7]

Diameter and albedo[edit]

According to the survey carried out by NASA's Wide-field Infrared Survey Explorer with its subsequent NEOWISE mission, Rubincam measures 4.250 kilometers in diameter and its surface has an albedo of 0.204,[4][5] while the Collaborative Asteroid Lightcurve Link assumes a standard albedo for stony asteroids of 0.20 and calculates a diameter of 4.1 kilometers with an absolute magnitude of 14.3.[3]

Naming[edit]

This minor planet was named after David Rubincam (born 1947), an American solid-earth geophysicist and planetary geodynamicist at NASA's Goddard Space Flight Center in Washington D.C. He was the first to study the influence of the radiation recoil effects on an asteroid's rotation period and spin axis, which he later named the Yarkovsky–O'Keefe–Radzievskii–Paddack effect or YORP effect for short.[2] The official naming citation was published by the Minor Planet Center on 28 September 2015 (M.P.C. 95803).[8]

References[edit]

  1. ^ a b c d "JPL Small-Body Database Browser: 9921 Rubincam (1981 EO18)" (2017-03-14 last obs.). Jet Propulsion Laboratory. Retrieved 22 June 2017. 
  2. ^ a b c d "9921 Rubincam (1981 EO18)". Minor Planet Center. Retrieved 10 April 2017. 
  3. ^ a b c d e f "LCDB Data for (9921) Rubincam". Asteroid Lightcurve Database (LCDB). Retrieved 10 April 2017. 
  4. ^ a b c d Mainzer, A.; Grav, T.; Masiero, J.; Hand, E.; Bauer, J.; Tholen, D.; et al. (November 2011). "NEOWISE Studies of Spectrophotometrically Classified Asteroids: Preliminary Results" (PDF). The Astrophysical Journal. 741 (2): 25. arXiv:1109.6407Freely accessible. Bibcode:2011ApJ...741...90M. doi:10.1088/0004-637X/741/2/90. Retrieved 10 April 2017. 
  5. ^ a b c 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. arXiv:1109.4096Freely accessible. Bibcode:2011ApJ...741...68M. doi:10.1088/0004-637X/741/2/68. Retrieved 10 April 2017. 
  6. ^ a b Polishook, D.; Ofek, E. O.; Waszczak, A.; Kulkarni, S. R.; Gal-Yam, A.; Aharonson, O.; et al. (April 2012). "Asteroid rotation periods from the Palomar Transient Factory survey". Monthly Notices of the Royal Astronomical Society. 421 (3): 2094–2108. arXiv:1201.1930Freely accessible. Bibcode:2012MNRAS.421.2094P. doi:10.1111/j.1365-2966.2012.20462.x. Retrieved 10 April 2017. 
  7. ^ 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 10 April 2017. 
  8. ^ "MPC/MPO/MPS Archive". Minor Planet Center. Retrieved 10 April 2017. 

External links[edit]