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

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

Nov 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011iaus..276..407d&link_type=abstract

The Astrophysics of Planetary Systems: Formation, Structure, and Dynamical Evolution, Proceedings of the International Astronomi

Astronomy and Astrophysics

Astrophysics

Accretion Disks, Turbulence, Mhd

Scientific paper

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.

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