Long-term stability of the dead-zone in proto-planetary disks

Details Long-term stability of the dead-zone in proto-planetary disks Long-term stability of the dead-zone in proto-planetary disks

Nov 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011iaus..276..418f&link_type=abstract

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

Astronomy and Astrophysics

Astrophysics

Accretion Disks, Mhd, Turbulence, Planetary Systems: Formation, Instabilities

Scientific paper

We present 3D global non-ideal MHD simulations with a self consistent dynamic evolution of ionization fraction of the gas as result of reduced chemical network. We include X-ray ionization from the star as well as cosmic ray ionization. Based on local gas density and temperature in our chemical network, we determine the magnetic resistivity, which is fed back in MHD simulations. Parameters for dust size and abundance are chosen to have accreting layers and a laminar ``dead'' mid-plane.

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