Origin of the obliquities of the giant planets in mutual interactions in the early Solar System

Details Origin of the obliquities of the giant planets in mutual interactions in the early Solar System Origin of the obliquities of the giant planets in mutual interactions in the early Solar System

Apr 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006natur.440.1163b&link_type=abstract

Nature, Volume 440, Issue 7088, pp. 1163-1165 (2006).

Physics

4

Scientific paper

The origin of the spin-axis orientations (obliquities) of the giant planets is a fundamental issue because if the obliquities resulted from tangential collisions with primordial Earth-sized protoplanets, then they are related to the masses of the largest planetesimals out of which the planets form. A problem with this mechanism, however, is that the orbital planes of regular satellites would probably be uncorrelated with the obliquities, contrary to observations. Alternatively, they could have come from an external twist that affected the orientation of the Solar System plane; but in this model, the outer planets must have formed too rapidly, before the event that produced the twist. Moreover, the model cannot be quantitatively tested. Here I show that the present obliquities of the giant planets were probably achieved when Jupiter and Saturn crossed the 1:2 orbital resonance during a specific migration process: different migration scenarios cannot account for the large observed obliquities. The existence of the regular satellites of the giant planets does not represent a problem in this model because, although they formed soon after the planetary formation, they can follow the slow evolution of the equatorial plane it produces.

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