Torques on Sedna by a Putative Massive Body in the Oort Cloud

Details Torques on Sedna by a Putative Massive Body in the Oort Cloud Torques on Sedna by a Putative Massive Body in the Oort Cloud

Nov 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004dps....36.0809m&link_type=abstract

American Astronomical Society, DPS meeting #36, #08.09; Bulletin of the American Astronomical Society, Vol. 36, p.1082

Physics

Geophysics

Scientific paper

Morbidelli and Levison (arXiv:astro-ph/0403358) consider various scenarios for the origin of the orbits of Sedna-like objects. The only one which they find to give satisfactory results is the passage of a low-velocity solar-mass star at about 800 AU during the early solar environment. They observe that creating ``extended scattered disk objects" (in which the largest orbits also have the largest q) requires a perturbation ``from the outside", but do not discuss the possibility that the external perturbation could come from a Jovian-mass wide-binary solar companion. We investigate the parameter space of such an object which would adiabatically detach Sedna from Neptune's dominance with qS (0) ≈ 30 AU, aS = 531 AU. Demanding that the detached osculating orbit satisfy qmin>15 AU, qmax >75 AU, the companion's mass and orbit parameters (m, a, e) that can produce n osculation cycles in a time Δ t are $(m)/(MJup)≈ n/tssΔ t (a)/(6000 AU)3(1-e^2)3/2. A wide-binary companion could also be the source of the 7^° misalignment of the ecliptic plane normal with the solar spin axis (Hogg, Quinlan and Tremaine 1991, Astron. J. 101(6), 2274), but only if n≈ 100$. The solar impulse considered by Morbidelli and Levison would produce an ecliptic plane tilt only 1/100 of that observed.
J.J.L. received support from Planetary Geology and Geophysics Grant 344-30-1L.

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