A low mass for Mars from Jupiter’s early gas-driven migration

Kevin J. Walsh (), Alessandro Morbidelli, Sean N. Raymond, David P. O'Brien and Avi M. Mandell
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Kevin J. Walsh: Université de Nice – Sophia Antipolis, CNRS, Observatoire de la Côte d'Azur, BP 4229, 06304 Nice Cedex 4, France
Alessandro Morbidelli: Université de Nice – Sophia Antipolis, CNRS, Observatoire de la Côte d'Azur, BP 4229, 06304 Nice Cedex 4, France
Sean N. Raymond: Université de Bordeaux, Observatoire Aquitain des Sciences de l'Univers, 2 Rue de l'Observatoire, BP 89, F-33270 Floirac Cedex, France
David P. O'Brien: Planetary Science Institute, 1700 East Fort Lowell, Suite 106, Tucson, Arizona 85719, USA
Avi M. Mandell: NASA Goddard Space Flight Center, Code 693, Greenbelt, Maryland 20771, USA

Nature, 2011, vol. 475, issue 7355, 206-209

Abstract: How Jupiter pulls the strings The giant planets formed much earlier in the life of the Solar System than the terrestrial ones, taking just a few million years to coalesce from the protoplanetary disk. They were also quite mobile, on timescales in the order of 100,000 years. Simulations of the early Solar System now show how an inward migration of Jupiter followed by an outward migration could have produced a truncated planetesimal disk from which terrestrial planets formed over the next 30–50 million years. The terrestrial planets stopped accreting much later, and their characteristics, including Mars's small mass, are best reproduced by starting from a planetesimal disk that has an outer edge at around one astronomical unit from the Sun.

Date: 2011
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DOI: 10.1038/nature10201

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