Accretion To Magnetized Stars Through The Rayleigh-taylor Instability: Global Three-dimensional Simulations

Details Accretion To Magnetized Stars Through The Rayleigh-taylor Instability: Global Three-dimensional Simulations Accretion To Magnetized Stars Through The Rayleigh-taylor Instability: Global Three-dimensional Simulations

Mar 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008head...10.1026k&link_type=abstract

American Astronomical Society, HEAD meeting #10, #10.26

Astronomy and Astrophysics

Astronomy

Scientific paper

We present results of 3D simulations of MHD instabilities at the accretion disk-magnetosphere boundary. The instability is Rayleigh-Taylor, and develops for a fairly broad range of accretion rates and stellar rotation rates and magnetic fields. It manifests itself in the form of tall, thin tongues of plasma that penetrate the magnetosphere in the equatorial plane. The shape and number of the tongues changes with time on the inner-disk dynamical timescale. In contrast with funnel flows, which deposit matter mainly in the polar region, the tongues deposit matter much closer to the stellar equator. The instability appears for relatively small misalignment angles, Θ

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