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2 - The Origin and Evolution of Saturn, with Exoplanet Perspective

Published online by Cambridge University Press:  13 December 2018

By
Sushil K. Atreya ,
Aurélien Crida ,
Tristan Guillot ,
Jonathan I. Lunine ,
Nikku Madhusudhan  and
Olivier Mousis
Edited by
Kevin H. Baines ,
F. Michael Flasar ,
Norbert Krupp  and
Tom Stallard
Kevin H. Baines
Affiliation:
University of Wisconsin, Madison
F. Michael Flasar
Affiliation:
NASA-Goddard Space Flight Center
Norbert Krupp
Affiliation:
Max-Planck-Institut für Sonnensystemforschung, Göttingen
Tom Stallard
Affiliation:
University of Leicester
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Summary

Saturn formed beyond the snow line in the primordial solar nebula, and that made it possible for it to accrete a large mass. Disk instability and core accretion models have been proposed for Saturn’s formation, but core accretion is favored on the basis of its volatile abundances, internal structure, hydrodynamic models, chemical characteristics of protoplanetary disk, etc. The observed frequency, properties, and models of exoplanets provide additional supporting evidence for core accretion. The heavy elements with mass greater than 4He make up the core of Saturn, but are presently poorly constrained, except for carbon. The C/H ratio is super-solar, and twice that in Jupiter. The enrichment of carbon and other heavy elements in Saturn and Jupiter requires special delivery mechanisms for volatiles to these planets. In this chapter we will review our current understanding of the origin and evolution of Saturn and its atmosphere, using a multi-faceted approach that combines diverse sets of observations on volatile composition and abundances, relevant properties of the moons and rings, comparison with the other gas giant planet, Jupiter, and analogies to the extrasolar giant planets, as well as pertinent theoretical models.

Type
Chapter
Information
Saturn in the 21st Century , pp. 5 - 43
Publisher: Cambridge University Press
Print publication year: 2018

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