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Planetesimal and protoplanet dynamics in a turbulent protoplanetary disk

Published online by Cambridge University Press:  10 November 2011

Chao-Chin Yang ,
Mordecai-Mark Mac Low  and
Kristen Menou
Chao-Chin Yang
Affiliation:
Department of Astronomy, University of Illinois, 1002 West Green Street, Urbana, IL 61801, U.S.A Department of Astrophysics, American Museum of Natural History, Central Park West at 79th Street, New York, NY 10024, U.S.A
Mordecai-Mark Mac Low
Affiliation:
Department of Astrophysics, American Museum of Natural History, Central Park West at 79th Street, New York, NY 10024, U.S.A
Kristen Menou
Affiliation:
Department of Astrophysics, American Museum of Natural History, Central Park West at 79th Street, New York, NY 10024, U.S.A
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Abstract

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Due to the gravitational influence of density fluctuations driven by magneto-rotational instability in the gas disk, planetesimals and protoplanets undergo diffusive radial migration as well as changes of other orbital properties. The magnitude of the effect on particle orbits has important consequences for planet formation scenarios. We use the local-shearing-box approximation to simulate an ideal, isothermal, magnetized gas disk with vertical density stratification and simultaneously evolve numerous massless particles moving under the gravity of the gas and the host star. Although the results converge with resolution for fixed box dimensions, we find there exists no convergence of the response of the particles to the gravity of the gas against the horizontal box size, up to 16 disk scale heights. This lack of convergence indicate that caution should be exercised when interpreting local-shearing-box models involving gravitational physics of magneto-rotational turbulence.

Keywords

accretionaccretion disksinstabilitiesmethods: numericalMHDplanetary systems: formationplanetary systems: protoplanetary disksturbulence
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 6 , Symposium S276: The Astrophysics of Planetary Systems: Formation, Structure, and Dynamical Evolution , October 2010 , pp. 517 - 518
Copyright
Copyright © International Astronomical Union 2011

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