Orbital Evolution of Extra-Solar Giant Planets

Details Orbital Evolution of Extra-Solar Giant Planets Orbital Evolution of Extra-Solar Giant Planets

Sep 1996

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996dps....28.1213t&link_type=abstract

American Astronomical Society, DPS meeting #28, #12.13; Bulletin of the American Astronomical Society, Vol. 28, p.1113

Astronomy and Astrophysics

Astronomy

2

Scientific paper

The recent discoveries (Mayor and Queloz, 1995; Marcy and Butler, 1996; Butler and Marcy, 1996) of extra-solar giant planets (EGPs) at small heliocentric distances have prompted questions about the formation, evolution, and migration of these EGPs. The location of several EGPs at much less than 1 AU from their primaries has proved to be particularly problematic. Since it is thought that EGPs do not form that close to their primaries (Guillot et al., 1996), a reasonable conclusion is that these close companions formed elsewhere in their solar systems and subsequently moved to their present small heliocentric distances. Jupiter-style planetary formation is thought to initiate at the ice line ( ~ several AU) (Boss, 1995), with possible subsequent inward migration (Lin and Papaloizou, 1986). But how can a massive body stop its inward migration before crashing into its star? We investigate the orbital evolution of an EGP with our fully implicit numerical model. Inward migration is caused by angular momentum exchange between the planet and disk (Takeuchi et al., 1996, Lin and Papaloizou, 1986). After the planet has migrated to much less than 1 AU, its inward motion can be halted by outward torques due to tides (Lin et al., 1996) and due to angular momentum exchange from Roche lobe overflow and mass loss (Benz et al., 1990). EGPs may stably survive, some at new, smaller masses, at small heliocentric distances for greater than 10(7) years, by which time the disk has dissipated (Zuckerman et al., 1995) and the torques have nearly vanished. This mechanism may explain the presence of EGPs at small heliocentric distances. References: Benz et al., 1990, Ap. J., 348, 647. Boss, 1995, Science, 267, 360. Butler and Marcy, 1996, Ap. J., 464, L153. Guillot et al., 1996, Ap. J., 459, L35. Lin et al., 1996, Nature, 380, 606. Lin and Papaloizou, 1986, Ap. J., 309, 846. Marcy and Butler, 1996, Ap. J., 464, L147. Mayor and Queloz, 1995, Nature, 378, 355. Takeuchi et al., 1996, Ap. J., 460, 832. Zuckerman et al., 1995, Nature, 373, 494. Acknowledgement: This work is supported in part under an NSF Graduate Research Fellowship.

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