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Three Dimensional MHD Simulations of Parker Instability in Differentially Rotating Disk

Published online by Cambridge University Press:  12 April 2016

T. Matsuzaki ,
R. Matsumoto ,
T. Tajima  and
K. Shibata
T. Matsuzaki
Affiliation:
Department of Physics, Faculty of Science, Chiba University, 1–33 Yayoi-Cho, Inage-Ku, Chiba 263, Japan
R. Matsumoto*
Affiliation:
Department of Physics, Faculty of Science, Chiba University, 1–33 Yayoi-Cho, Inage-Ku, Chiba 263, Japan
T. Tajima
Affiliation:
Institute for Fusion Studies, University of Texasat Austin, Austin, TX 78712, USA
K. Shibata
Affiliation:
National Astronomical Obserbatory, Mitaka, Tokyo 181, Japan
*
Advanced Science Research Center, JAERI, Naka, Japan

Abstract

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Nonlinear growth of the Parker instability (PI) and the Balbus & Hawley instability (BHI) in accretion disks have been studied by local three-dimensional magnetohydrodynamic (MHD) simulations. In high-β disks (β = Pgas/Pmag > 1), the PI has only minor effects on the saturation level of BHI. In low β disks (β ≤ 1), the disk stays in a low-β state because magnetic flux cannot escape fast enough to convert the disk into a high-β state. We found that even in low-β disk the BHI generates fluctuating magnetic fields. The effective magnetic viscosity αB(= –⟨BrBΦ/4πP0⟩) is O(0.1) when β ~ 1.

Type
Part 15. Poster Papers
Information
International Astronomical Union Colloquium , Volume 163: Accretion Phenomena and Related Outflows , 1997 , pp. 766 - 767
Copyright
Copyright © Astronomical Society of the Pacific 1997

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