Resonances near the orbit of 2003 VB_{12} (Sedna)

Details Resonances near the orbit of 2003 VB_{12} (Sedna) Resonances near the orbit of 2003 VB_{12} (Sedna)

Feb 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005dpps.conf..341c&link_type=abstract

Dynamics of Populations of Planetary Systems, Proceedings of IAU Colloquium #197, held 31 August - 4 Spetember, 2004 in Belgrade

Physics

1

Celestial Mechanics, Kuiper Belt, Minor Planets, Asteroids, Oort Cloud, Solar System: Formation.

Scientific paper

2003 VB_{12} (Sedna) is as much distinguished by its considerable size as by its extremely unusual orbit, which has perihelion at about q=76 AU with semi-major axis a=533 AU (Brown et al. 2004, JPL Horizons). Thus it is effectively decoupled from both Neptune and the Galactic tide (Fernandez 1997). Brown et al. (2004) and Morbidelli & Levison (2004) maintain that only scattering by a so-far-unobserved “Planet X” or by an errant star could produce such a high-perihelion orbit for a scattered-disk KBO. While a close encounter is plausible, given the Sun's likely birth in an open cluster, such an interaction would profoundly disturb the Oort cloud and would require fundamental revision to the present theories of its formation.

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