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T. Tanigawa (Tokyo Institute of Technology), D.N.C. Lin (UC Santa Cruz)
We carry out hydrodynamic simulations of a proto-planetary disk with an embedded low-mass proto-planet in order to investigate the effect of self gravity of the disk on the migration velocity of the planet. For the disk model, we adopt power functions for the surface density profile and the temperature profile. We investigate the dependence on various parameters, such as the exponents of power functions of temperature and surface density, disk mass, and planet mass. We find that, without self gravity, the dependence of the planet mass on the torque is qualitatively agree with linear analysis of Tanaka, Takeuchi and Ward 2002. With self-gravity cases, the dependence of the disk surface density on the torque is slightly stronger than linear relationship, which infers that the effect of self gravity could accelerate inward migration of planets. This research is supported by the Ministry of Education, Culture, Sports, Science and Technology (MEXT 16077202).
The author(s) of this abstract have provided an email address for comments about the abstract: tanigawa@geo.titech.ac.jp
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Bulletin of the American Astronomical Society, 37 #3
© 2004. The American Astronomical Soceity.