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MHD instabilities at the disk-magnetosphere boundary: 3D simulations

Published online by Cambridge University Press:  01 May 2007

Akshay K. Kulkarni  and
Marina M. Romanova
Akshay K. Kulkarni
Affiliation:
Department of Astronomy, Cornell University, Ithaca, NY 14853, USA email: akshay@astro.cornell.edu, romanova@astro.cornell.edu
Marina M. Romanova
Affiliation:
Department of Astronomy, Cornell University, Ithaca, NY 14853, USA email: akshay@astro.cornell.edu, romanova@astro.cornell.edu
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Abstract

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We present results of 3D simulations of MHD instabilities at the accretion disk-magnetosphere boundary. The instability is Rayleigh-Taylor, and develops for a large range of parameter values. It manifests itself in the form of tall, thin tongues of plasma that reach the star by penetrating through the magnetosphere in the equatorial plane. The tongues rotate around the star in the equatorial plane, and their shape and number changes with time on inner-disk dynamical timescales. In contrast with funnel flows, which deposit matter mainly in the polar region, the tongues deposit matter much closer to the stellar equator.

Keywords

Accretionaccretion disksinstabilities(magnetohydrodynamics:) MHDstars: circumstellar matterstars: magnetic fieldsstars: oscillationsstars: pre-main-sequencestars: rotationstars: spots
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 3 , Symposium S243: Star-Disk Interaction in Young Stars , May 2007 , pp. 291 - 298
Copyright
Copyright © International Astronomical Union 2007

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