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Magnetic Field Reconnection in Differentially Rotating Accretion Disks

Published online by Cambridge University Press:  04 August 2017

David Gilden  and
T. Tajima
David Gilden
Affiliation:
The Institute for Advanced Study
T. Tajima
Affiliation:
Institute for Fusion Studies, University of Texas at Austin

Abstract

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Differentially rotating accretion disks threaded by a uniform magnetic field have been numerically simulated. Fast reconnection followed by coalescence allows the magnetic field to drive small amplitude radial oscillations in the disk. These oscillations may be observable as the viscous stresses cause the disk to brighten and fade as the disk expands and contracts. Episodes of reconnection may also be observable as hot spots produced locally at the sites of coalescence. Cataclysmic variables, and in particular dwarf novae, provide a natural interpretation for these calculations.

Type
Session VII
Information
Symposium - International Astronomical Union , Volume 107: Unstable Current Systems and Plasma Instabilities , 1985 , pp. 477 - 482
Copyright
Copyright © Reidel 1985 

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