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The effect of poloidal magnetic field on type I planetary migration

Published online by Cambridge University Press:  01 October 2007

Takayuki Muto ,
Masahiro N. Machida  and
Shu-ichiro Inutsuka
Takayuki Muto
Affiliation:
Department of Physics, Kyoto University, Kitashirakawa-Oiwake-Cho, Sakyo-ku, Kyoto, 606-8502, JAPAN email: muto@tap.scphys.kyoto-u.ac.jp
Masahiro N. Machida
Affiliation:
Department of Physics, Kyoto University, Kitashirakawa-Oiwake-Cho, Sakyo-ku, Kyoto, 606-8502, JAPAN email: muto@tap.scphys.kyoto-u.ac.jp
Shu-ichiro Inutsuka
Affiliation:
Department of Physics, Kyoto University, Kitashirakawa-Oiwake-Cho, Sakyo-ku, Kyoto, 606-8502, JAPAN email: muto@tap.scphys.kyoto-u.ac.jp
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Abstract

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We study the effect of poloidal magnetic field on type I planetary migration by linear perturbation analysis with the shearing-sheet approximation and the analytic results are compared with numerical calculation. We investigate the cases where magneto-rotational instability (MRI) does not occur: either the disk is two-dimensional, or a very strong field is exerted. We derive formulae for torque exerted on the planet for both cases. We find that two-dimensional torque is suppressed when plasma beta is less than 1 and three-dimensional modes dominate, in contrast to unmagnetized case.

Keywords

MHD — planets and satellites: formation — solar system: formation
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 3 , Symposium S249: Exoplanets: Detection, Formation and Dynamics , October 2007 , pp. 401 - 406
Copyright
Copyright © International Astronomical Union 2008

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