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MHD simulations of star-disk magnetospheres and the formation of outflows and jets

Published online by Cambridge University Press:  01 May 2007

Christian Fendt
Christian Fendt*
Affiliation:
Max Planck Institute for Astronomy, Königstuhl 17, 69117 Heidelberg, Germany email: [email protected]
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Abstract

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In this review the recent development concerning the large-scale evolution of stellar magnetospheres in interaction with the accretion disk is discussed. I put emphasis on the generation of outflows and jets from the disk and/or the star. In fact, tremendous progress has occurred over the last decade in the numerical simulation of the star-disk interaction. The role of numerical simulations is essential in this area because the processes involved are complex, strongly interrelated, and often highly time-dependent. Recent MHD simulations suggest that outflows launched from a very concentrated region tend to be un-collimated. I present preliminary results of simulations of large-scale star-disk magnetospheres loaded with matter from the stellar, resp. the disk surface demonstrating how a disk jet collimates the wind from the star and also how the stellar wind lowers the collimation degree of the disk outflow.

Keywords

Accretion disksMHDmethods: numericalstars: formationstars: magnetic fieldsstars: mass lossstars: windsoutflowsISM: jets and outflows
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 3 , Symposium S243: Star-Disk Interaction in Young Stars , May 2007 , pp. 265 - 276
Copyright
Copyright © International Astronomical Union 2007

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