2013 RF98

2013 RF98 is a trans-Neptunian object.[2] It was discovered on September 12, 2013 at Cerro Tololo-DECam

2013 RF98
Discovery[1]
Discovered byDark Energy Survey (807)
Discovery date12 September 2013
Designations
Designation
2013 RF98
TNO
Orbital characteristics[2]
Epoch 16 February 2017 (JD 2457800.5)
Uncertainty parameter 5
Observation arc1092 days (2.99 yr)
Aphelion662 ± 20 AU (Q)
690 AU (barycentric)[3]
Perihelion36.09 0.03 AU (q)
349 ± 11 AU
364 AU (barycentric)[3]
Eccentricity0.897 ± 0.003
6527 ± 299 yr
6900 yr (barycentric solution)[3]
0.404° ± 0.004°
Inclination29.572° ± 0.003°
67.596° ± 0.005°
311.8° ± 0.6°
Physical characteristics
Dimensions~50-120 km
Spectral type
Blue[4]
24.4 (2016)
28.8 (@100AU)
8.7 ± 0.3[2]

    It is part of the evidence for the Planet Nine hypothesis because it shares a similar argument of perihelion with other potentially shepherded TNOs.

    Discovery, orbit and physical properties
    2013 RF98 orbit in green (upper left) with hypothetical Planet Nine

    2013 RF98 was discovered by the Dark Energy Survey on September 12, 2013 observing with the 4 m Blanco Telescope from Cerro Tololo Inter-American Observatory.[1] Its orbit is characterized by high eccentricity (0.897), moderate inclination (29.57º) and a semi-major axis of 349 AU.[1] Upon discovery, it was classified as a trans-Neptunian object. Its orbit is relatively well determined; as of January 11, 2017 its orbital solution is based on 51 observations spanning a data-arc of 1092 days.[2] 2013 RF98 has an absolute magnitude of 8.7 which gives a characteristic diameter of 50 to 120 km for an assumed albedo in the range 0.25–0.05.[5]

    It came to perihelion (closest approach to the Sun) around October 2009 and was last observed in September 2016.[2] As of October 2016, it is 36.6 AU from the Sun. Of the seven objects whose aligned orbits suggest the existence of Planet Nine, it is currently the closest to the Sun. It will be 18.7 AU from Uranus in 2021. It will be in the constellation of Cetus until 2022. It comes to opposition at the start of November.

    2013 RF98's orbit is similar to that of (474640) 2004 VN112, suggesting that they may have both been thrown onto their current paths by the same body, or that they may have been the same object (single or binary) at one point.[4][6]

    2013 RF98's visible spectrum is very different from that of 90377 Sedna.[4][7] The value of its spectral slope suggests that the surface of this object can have pure methane ices (like in the case of Pluto) and highly processed carbons, including some amorphous silicates.[4] Its spectral slope is similar to that of 2004 VN112.[4]

    See also

    References
    1. "List Of Centaurs and Scattered-Disk Objects". Minor Planet Center. Retrieved 22 January 2016.
    2. "JPL Small-Body Database Browser: (2013 RF98)" (last observation: 2016-10-08; arc: 1092 days). Jet Propulsion Laboratory. Archived from the original on 23 January 2016. Retrieved 22 October 2016.
    3. Horizons output. "Barycentric Osculating Orbital Elements for 2013 RF98". Retrieved 8 February 2017. (Ephemeris Type:Elements and Center:@0)
    4. de León, Julia; de la Fuente Marcos, Carlos; de la Fuente Marcos, Raúl (May 2017). "Visible spectra of (474640) 2004 VN112-2013 RF98 with OSIRIS at the 10.4 m GTC: evidence for binary dissociation near aphelion among the extreme trans-Neptunian objects". Monthly Notices of the Royal Astronomical Society: Letters. 467 (1): L66–L70. arXiv:1701.02534. Bibcode:2017MNRAS.467L..66D. doi:10.1093/mnrasl/slx003. S2CID 119419889.
    5. "ABSOLUTE MAGNITUDE (H)". NASA/JPL. Retrieved 28 February 2008.
    6. de la Fuente Marcos, C.; de la Fuente Marcos, R.; Aarseth, S. J. (1 November 2017). "Binary stripping as a plausible origin of correlated pairs of extreme trans-Neptunian objects". Astrophysics and Space Science. 362 (11): 198 (18pp.). arXiv:1709.06813. Bibcode:2017Ap&SS.362..198D. doi:10.1007/s10509-017-3181-1. S2CID 118890903.
    7. "JPL Small-Body Database Browser: 90377 Sedna (2003 VB12)". Retrieved 28 March 2014.
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