Astronomy and Astrophysics – Astronomy
Scientific paper
Sep 2009
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009dps....41.5502b&link_type=abstract
American Astronomical Society, DPS meeting #41, #55.02
Astronomy and Astrophysics
Astronomy
Scientific paper
Giant planets are expected to be born on quasi-circular orbits, which are further damped by the interaction with the disc of gas from which they form, so that their eccentricities should have been acquired later. For a successful model that reconstructs the observed eccentricities of the planets, not only should the mean values be reproduced, but also the amplitude of each eigenmode present in the eccentricity spectrum.
Giant planets:
We show that, at the very least, encounters between Saturn and one of the ice giants need to have occurred, in order to reproduce the current secular properties of the giant planets, in particular the amplitude of the two main eigenmodes in the eccentricity spectrum of Jupiter and Saturn.
Terrestrial planets:
The divergent migration of Jupiter and Saturn causes the crossing of secular resonances of the form g5=gk with k from 1-4. The g5=g4 and g5=g3 resonances are not a problem if Jupiter and Saturn started beyond their 2:1 resonance or quickly crossed it. However, the resonances g5=g2 and g5=g1 are of concern because they yield a terrestrial system incompatible with the current one: the amplitudes of the g1 and g2 modes are too large. We present two solutions for this problem. First, a secular resonance crossing can damp the amplitude of a Fourier mode if the latter is large originally. Second, a 'jumping Jupiter' evolution in which encounters between an ice giant and Jupiter, without ejection of the former, cause the latter to migrate away from Saturn much faster than if migration is driven solely by encounters with planetesimals. In this case, the g5=g2 and g5=g1 resonances can be jumped over, or occur very briefly.
Brasser Ramon
Gomes Rodney
Levison Hal
Morbidelli Alessandro
Tsiganis Kleomenis
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