Reversing Type I Migration in Gap Shadows

Details Reversing Type I Migration in Gap Shadows Reversing Type I Migration in Gap Shadows

Sep 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011ess.....2.1607j&link_type=abstract

American Astronomical Society, ESS meeting #2, #16.07

Astronomy and Astrophysics

Astronomy

Scientific paper

Type I migration refers to the radial drift of a planet resulting from tidal interactions with a protoplanetary disk. It results in rapid inward migration of a planet through a disk and may explain the preponderance of hot Jupiters in inventory of known exoplanets. However, Type I migration is so rapid compared to disk dissipation that explaining distant gas giant planets, such as the HR 8799 planets and Jupiter itself, is problematic. Here, we present a scenario for solving the Type I migration problem. As a planet grows in mass, its Type I migration rate increases. It also begins to clear material from its orbital path, creating a gap in the disk. The trough of such partially cleared gaps is shadowed from stellar illumination while the far side of the gap is illuminated. Since stellar irradiation is the primary heat source of passively accreting protoplanetary disks, gap self-shadowing can significantly change the local temperature profile. This change to the local temperature gradient can significantly slow, or even reverse Type I migration.

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