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MHD simulations of disk-star interaction

Published online by Cambridge University Press:  01 May 2007

Marina M. Romanova
Affiliation:
Astronomy Department, Cornell University, Ithaca, NY 14853, USA; email: [email protected]
M. Long
Affiliation:
Astronomy Department, Cornell University, Ithaca, NY 14853, USA; email: [email protected]
A. K. Kulkarni
Affiliation:
Astronomy Department, Cornell University, Ithaca, NY 14853, USA; email: [email protected]
R. Kurosawa
Affiliation:
Department of Physics and Astronomy, University of Nevada Las Vegas, Box 454002, 4505 Maryland Pkwy, Las Vegas, NV 89154-4002, USA; email: [email protected]
G. V. Ustyugova
Affiliation:
Keldysh Institute of Applied Mathematics, Miusskaya sq. 4, Moscow, 125047, Russia, email: [email protected]
A. K. Koldoba
Affiliation:
Keldysh Institute of Applied Mathematics, Miusskaya sq. 4, Moscow, 125047, Russia, email: [email protected]
R. V. E. Lovelace
Affiliation:
Astronomy Department, Cornell University, Ithaca, NY 14853, USA; email: [email protected]
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Abstract

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We discuss a number of topics relevant to disk-magnetosphere interaction and how numerical simulations illuminate them. The topics include: (1) disk-magnetosphere interaction and the problem of disk-locking; (2) the wind problem; (3) structure of the magnetospheric flow, hot spots at the star's surface, and the inner disk region; (4) modeling of spectra from 3D funnel streams; (5) accretion to a star with a complex magnetic field; (6) accretion through 3D instabilities; (7) magnetospheric gap and survival of protoplanets. Results of both 2D and 3D simulations are discussed.

Type
Contributed Papers
Copyright
Copyright © International Astronomical Union 2007

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