WALSH, Kevin J.; MORBIDELLI, Alessando; RAYMOND, Sean N.; O'BRIEN, David P.; MANDELL, Avi M.

doi:10.1017/S1743921313012854

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WALSH, Kevin J.

MORBIDELLI, Alessando

RAYMOND, Sean N.
SSE 2014

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Communication dans un congrès

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Proceedings of the International Astronomical Union, Formation, Detection, and Characterization of Extrasolar Habitable Planets, Proceedings of the International Astronomical Union, IAU Symposium, held in China, August 27, 2012, - Volume 293, pp. 204-211, 2014, Formation, Detection, and Characterization of Extrasolar Habitable Planets, Proceedings of the International Astronomical Union, IAU Symposium, held in China, August 27, 2012, - Volume 293, pp. 204-211, 2014, 2012, Beijing. 2014-04, vol. 293, p. 204-211

Cambridge University Press (CUP)

Resumen en inglés

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.< Leer menos

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

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