Magnetic buoyancy in accretion disks

Details Magnetic buoyancy in accretion disks Magnetic buoyancy in accretion disks

Jul 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993a%26a...274..675t&link_type=abstract

Astronomy and Astrophysics, Vol. 274, p. 675 (1993)

Astronomy and Astrophysics

Astrophysics

5

Accretion, Accretion Disks, Instabilities, Magnetic Fields, Mhd

Scientific paper

The expulsion of flux tubes from an accretion disk due to magnetic buoyancy is studied. The vertical structure of the disk is assumed to be either isothermal or polytropic. The flux tube is constrained to move vertically. Initially it is at rest and in thermal equilibrium with the surrounding plasma at the disk equator. It is then given a small velocity, and the subsequent evolution is followed. To simplify the calculations it is assumed that the flux tube either remains in thermal equilibrium with its environment or is moving adiabatically. These calculations are repeated for a polytropic accretion disk surrounded by a hot and tenuous isothermal corona. It is found that the corona stabilizes the buoyant flux tubes. By comparing my results with Sakimoto & Coroniti (1989), I come to the conclusion that radiative transport of heat is not important for the behaviour of the flux tube. Finally I discuss effects limiting the validity of the model and the astrophysical implications of the model.

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