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3D global simulations of proto-planetary disk with dynamically evolving outer edge of dead zone

Published online by Cambridge University Press:  10 November 2011

Natalia Dzyurkevich ,
Neal J. Turner ,
Willy Kley ,
Hubert Klahr  and
Thomas Henning
Natalia Dzyurkevich
Affiliation:
Max-Planck Institute for Astronomy, Königstuhl 17, Heidelberg, D-69117 email: natalia@mpia.de
Neal J. Turner
Affiliation:
Jet Propulsion Laboratory, California 91109, USA
Willy Kley
Affiliation:
University of Tübingen, Auf der Morgenstelle 10, Tübingen, D-72076
Hubert Klahr
Affiliation:
Max-Planck Institute for Astronomy, Königstuhl 17, Heidelberg, D-69117 email: natalia@mpia.de
Thomas Henning
Affiliation:
Max-Planck Institute for Astronomy, Königstuhl 17, Heidelberg, D-69117 email: natalia@mpia.de
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Abstract

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3D global MHD simulations of magneto-driven turbulence are performed for the disk of 100 AU with reduced amount of 10μm fluffy dust grains. We use X-ray and cosmic ray ionization, as well as simplified treatment of recombination on dust grains. The ionization of gas and charging of dust grains are dynamically evolving during the simulation, making the zone of high magnetic dissipation (’dead’ zone) variable. In our simulations, the jump in MRI-driven turbulent viscosity inside and outside of dead zone is insignificant. We find no hard edge, but rather a smooth transition between active and dead zone. Subsequently, there is no visible pressure bump at outer edge of the dead zone.

Keywords

accretion disksturbulenceMHD
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. 407 - 408
Copyright
Copyright © International Astronomical Union 2011

References

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