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The Obliquity of Jupiter

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Published 2006 February 28 © 2006. The American Astronomical Society. All rights reserved. Printed in U.S.A.
, , Citation William R. Ward and Robin M. Canup 2006 ApJ 640 L91 DOI 10.1086/503156

1538-4357/640/1/L91

Abstract

The spin-axis precession period of Jupiter is near that of a fundamental Laplace-Lagrange solar system mode describing the precession of Uranus's orbit plane (~4.3 × 105 yr). As a result, a portion of the 3fdg1 obliquity of Jupiter may actually be forced by a spin-orbit secular resonance with Uranus. If this portion predominates, it allows for a constraint on Jupiter's moment of inertia that is independent of interior models.

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10.1086/503156