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Shaping of the Inner Solar System by the Gas-Driven Migration of Jupiter

Published online by Cambridge University Press:  29 April 2014

Kevin J. Walsh ,
Alessando Morbidelli ,
Sean N. Raymond ,
David P. O'Brien  and
Avi M. Mandell
Kevin J. Walsh
Affiliation:
Southwest Research Institute1050 Walnut St. Suite 400, Boulder, CO, 80302, USA email: [email protected]
Alessando Morbidelli
Affiliation:
Obs. Côte d'Azur, Nice, France
Sean N. Raymond
Affiliation:
Lab. d'Astrophysique de Bordeaux, FloiracFrance
David P. O'Brien
Affiliation:
Planetary Science Institute, Tucson, AZ, USA
Avi M. Mandell
Affiliation:
NASA Goddard, Greenbelt, MD, USA
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Abstract

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A persistent difficulty in terrestrial planet formation models is creating Mars analogs with the appropriate mass: Mars is typically an order of magnitude too large in simulations. Some recent work found that a small Mars can be created if the planetesimal disk from which the planets form has an outermost edge at 1.0 AU. However, that work and no previous work could produce a truncation of the planetesimal disk while also explaining the mass and structure of the asteroid belt. We show that gas-driven migration of Jupiter inward to 1.5 AU, before its subsequent outward migration, can truncate the disk and repopulate the asteroid belt. This dramatic migration history of Jupiter suggests that the dynamical behavior of our giant planets was more similar to that inferred for extra-solar planets than previously thought, as both have been characterised by substantial radial migration.

Keywords

Planet FormationPlanet MigrationAsteroid Belt
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 8 , Symposium S293: Formation, Detection, and Characterization of Extrasolar Habitable Planets , August 2012 , pp. 204 - 211
Copyright
Copyright © International Astronomical Union 2014 

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