MHD Models of Accretion, Protostellar and Protoplanetary Disks

Details MHD Models of Accretion, Protostellar and Protoplanetary Disks MHD Models of Accretion, Protostellar and Protoplanetary Disks

Aug 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007jena.confe..92d&link_type=abstract

"JENAM-2007, "Our non-stable Universe", held 20-25 August 2007 in Yerevan, Armenia. Abstract book, p. 92-92"

Computer Science

Scientific paper

The base results of analytical and numerical investigations of accretion and protoplanetary disks formation around the young stars are discussed. The 2D MHD simulations of the protostellar clouds collapse show that binary or multiple protostars can form in the fast rotating clouds with the weak magnetic field. In the slow rotating clouds with the strong magnetic field the formation of single protostars with the accretion disks is more preferable. The formation of magnetostatic disk (MSTD) is possible when the initial magnetic energy is comparable with the gravitational one. The properties of accretion disks around T Tauri stars are studied in the framework of the generalized Shakura-Sunyaev MHD-model. It is shown that the intensive generation of the toroidal magnetic field component constrains the outer radius of accretion disk to the distances of the order 10^3 AU. The ambipolar and Ohmic diffusion determine the base parameters of a “dead zone” containing no dust, where the formation of massive gas planets is possible. Outside this zone the solid planets can form. The appearance of a current sheet in the magnetopause slows down the accretion rate in 5-10 times and renders the accretion disk into the state of a protoplanetary disk. In the magnetopause region can form the current sheet that can generate the X-Ray's radiation.

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