(309239) 2007 RW10

From Wikipedia, the free encyclopedia
Jump to navigation Jump to search
(309239) 2007 RW10
Discovered byPDSSS
Discovery date9 September 2007
TNO[1] · Nept. co-orbital
centaur · distant
Orbital characteristics[1]
Epoch 23 March 2018 (JD 2458200.5)
Uncertainty parameter 2
Observation arc10693 days (29.28 yr)
Aphelion39.28320 AU (5.876683 Tm)
Perihelion21.06436 AU (3.151183 Tm)
30.17878 AU (4.514681 Tm)
165.79 yr (60555.1 d)
0° 0m 21.402s / day
Earth MOID20.2499 AU (3.02934 Tm)
Jupiter MOID17.1323 AU (2.56296 Tm)
Physical characteristics
Dimensions247±30 km[2]

(309239) 2007 RW10, provisionally known as 2007 RW10, is a temporary quasi-satellite of Neptune.[3] Observed from Neptune, it would appear to go around it during one Neptunian year but it actually orbits the Sun, not Neptune.

Discovery, orbit and physical properties[edit]

(309239) 2007 RW10 was discovered by the Palomar Distant Solar System Survey on September 9, 2007,[4][5] with precovery images from 1988 (also taken at Palomar).[6] At the time of discovery, this minor body was believed to be a Neptune trojan,[7] but it is no longer listed as such.[8][9] The Jet Propulsion Laboratory classifies (309239) 2007 RW10 as trans-Neptunian object but the Minor Planet Center includes the object among centaurs. It moves in an orbit with an inclination of 36.2°, a semi-major axis of 30.18 AU, and an eccentricity of 0.3020.[1] Herschel-PACS observations indicate that it has a diameter of 247 km.[2]

Quasi-satellite dynamical state and orbital evolution[edit]

(309239) 2007 RW10 is currently following a quasi-satellite loop around Neptune.[3] It has been a quasi-satellite of Neptune for about 12,500 years and it will remain in that dynamical state for another 12,500 years.[3] Prior to the quasi-satellite dynamical state, (309239) 2007 RW10 was an L5 trojan and it will go back to that state soon after leaving its current quasi-satellite orbit. Its orbital inclination is the largest among known Neptune co-orbitals. It is also possibly the largest known object trapped in the 1:1 mean-motion resonance with any major planet.


(309239) 2007 RW10 is a dynamically hot (both, high eccentricity and inclination) object that is unlikely to be a primordial Neptune co-orbital. It probably originated well beyond Neptune and was later temporarily captured in the 1:1 commensurability with Neptune.[3][10]

See also[edit]

  • 2005 TN74, which was also suspected of being a Neptune trojan at the time of discovery


  1. ^ a b c d "JPL Small-Body Database Browser: 2007 RW10". Retrieved 2018-08-25.
  2. ^ a b c Santos-Sanz, P., Lellouch, E., Fornasier, S., Kiss, C., Pal, A., Müller, T. G., Vilenius, E., Stansberry, J., Mommert, M., Delsanti, A., Mueller, M., Peixinho, N., Henry, F., Ortiz, J. L., Thirouin, A., Protopapa, S., Duffard, R., Szalai, N., Lim, T., Ejeta, C., Hartogh, P., Harris, A. W., & Rengel, M. (2012). “TNOs are Cool”: A Survey of the Transneptunian Region IV - Size/albedo characterization of 15 scattered disk and detached objects observed with Herschel Space Observatory-PACS
  3. ^ a b c d de la Fuente Marcos, C.; de la Fuente Marcos, R. (2012). "(309239) 2007 RW10: a large temporary quasi-satellite of Neptune". Astronomy and Astrophysics Letters. 545: L9. arXiv:1209.1577. Bibcode:2012A&A...545L...9D. doi:10.1051/0004-6361/201219931.
  4. ^ "Discovery MPEC". Retrieved 2012-07-26.
  5. ^ Schwamb, Megan E.; et al. (September 2010). "Properties of the Distant Kuiper Belt: Results from the Palomar Distant Solar System Survey". The Astrophysical Journal. arXiv:1007.2954. Bibcode:2010ApJ...720.1691S. doi:10.1088/0004-637X/720/2/1691.
  6. ^ "(309239) = 2007 RW10". Retrieved 2018-08-25.
  7. ^ "Distant EKOs, 55". Retrieved 2012-07-24.
  8. ^ "Distant EKOs 56". Retrieved 2012-07-24.
  9. ^ Minor Planet Center List Of Neptune Trojans (2007-12-01)
  10. ^ Horner, J.; Lykawka, P. S.; Bannister, M. T.; Francis, P. (2012). "2008 LC18: a potentially unstable Neptune Trojan". Monthly Notices of the Royal Astronomical Society. 422 (3): 2145–2151. arXiv:1202.3279. Bibcode:2012MNRAS.422.2145H. doi:10.1111/j.1365-2966.2012.20757.x.

External links[edit]