(309239) 2007 RW10

(309239) 2007 RW10
Discovery
Discovered by PDSSS
Discovery date 9 September 2007
Designations
trans-Neptunian object
Orbital characteristics[1]
Epoch 13 January 2016 (JD 2457400.5)
Uncertainty parameter 3
Observation arc 8154 days (22.32 yr)
Aphelion 39.20412 AU (5.864853 Tm)
Perihelion 21.11597 AU (3.158904 Tm)
30.16005 AU (4.511879 Tm)
Eccentricity 0.29987
165.64 yr (60498.8 d)
66.98319°
0° 0m 21.422s / day
Inclination 36.17157°
187.07311°
95.68475°
Earth MOID 20.3005 AU (3.03691 Tm)
Jupiter MOID 17.1805 AU (2.57017 Tm)
Jupiter Tisserand parameter 3.881
Physical characteristics
Dimensions 247±30 km[2]
0.083+0.068
−0.039[2]
6.6[1]

    (309239) 2007 RW10, also written (309239) 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

    (309239) 2007 RW10 was discovered by the Palomar Distant Solar System Survey on September 9, 2007.[4][5] At the time of discovery, this minor body was believed to be a Neptune trojan,[6] but it is no longer listed as such.[7][8] 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 36.1°, a semi-major axis of 30.32 AU, and an eccentricity of 0.2996.[1] Herschel-PACS observations indicate that it has a diameter of 247 km.[2]

    Quasi-satellite dynamical state and orbital evolution

    (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.

    Origin

    (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][9]

    See also

    References

    1. 1 2 3 "JPL Small-Body Database Browser: 2007 RW10". Retrieved 8 April 2016.
    2. 1 2 3 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. 1 2 3 4 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:1209.1577Freely accessible. 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". arXiv:1007.2954Freely accessible. Bibcode:2010ApJ...720.1691S. doi:10.1088/0004-637X/720/2/1691. Retrieved 2012-07-26.
    6. ↑ "Distant EKOs, 55". Retrieved 2012-07-24.
    7. ↑ "Distant EKOs 56". Retrieved 2012-07-24.
    8. ↑ Minor Planet Center List Of Neptune Trojans (2007-12-01)
    9. ↑ 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, Volume 422, pp. 2145-2151

    External links

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