Tidal and Magnetic Interactions Between a Hot Jupiter and its Host Star in the Magnetospheric Cavity of a Protoplanetary Disk

We present a simplified model to study the orbital evolution of a young hot Jupiter inside the magnetospheric cavity of a proto-planetary disk. The model takes into account the disk locking of stellar spin as well as the tidal and magnetic interactions between the star and the planet. We focus on th...

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Bibliographic Details
Published in:The Astrophysical journal 2010-01, Vol.708 (2), p.1692-1702
Main Authors: Chang, S.-H, Gu, P.-G, Bodenheimer, P. H
Format: Article
Language:English
Subjects:
Astronomy
ASTROPHYSICS, COSMOLOGY AND ASTRONOMY
DWARF STARS
Earth, ocean, space
EVOLUTION
Exact sciences and technology
JUPITER PLANET
MASS
ORBITS
PLANETS
POTENTIALS
PROTOPLANETS
ROCHE EQUIPOTENTIALS
SIMULATION
STAR EVOLUTION
STARS
TORQUE
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Summary:We present a simplified model to study the orbital evolution of a young hot Jupiter inside the magnetospheric cavity of a proto-planetary disk. The model takes into account the disk locking of stellar spin as well as the tidal and magnetic interactions between the star and the planet. We focus on the orbital evolution starting from the orbit in 2:1 resonance with the inner edge of the disk, followed by the inward and then outward orbital migration driven by the tidal and magnetic torques as well as the Roche-lobe overflow of the tidally inflated planet. The goal in this paper is to study how the orbital evolution inside the magnetospheric cavity depends on the cavity size, planet mass, and orbital eccentricity. In the present work, we only target the mass range from 0.7 to 2 Jupiter masses. In the case of the large cavity corresponding to the rotational period 7 days, the planet of mass >1 Jupiter mass with moderate initial eccentricities (0.3) can move to the region
ISSN:0004-637X
1538-4357
DOI:10.1088/0004-637X/708/2/1692