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Three-Dimensional Local MHD Simulations of High States and Low States in Magnetic Accretion Disks

Published online by Cambridge University Press:  25 May 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, the University of Texas at Austin, Austin, TX 78712, USA
K. Shibata
Affiliation:
National Astronomical Observatory, Mitaka, Tokyo 181, Japan

Extract

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Black hole candidates sometimes show a transition between the high (or soft) state and the low (or hard) state. In the low state, low frequency time variations are much larger than the high state. A possible mechanism of the large-amplitude, sporadic time variabilities in the low-state is the magnetic energy release in low-β (β = Pgas/Pmag < 1) disks (Mineshige, Kusunose & Matsumoto 1995). It had been thought that low-β disks cannot exist because buoyant escape of magnetic flux due to the Parker instability may set the lower limit for β inside the disk. Shibata, Tajima & Matsumoto (1990), however, pointed out that in accretion disks, once a low-β disk is formed, it can stay in low-β state partly because the growth rate of the Parker instability decreases when β < 1. They suggested that magnetic accretion disks fall into two types; high-β disks and low-β disks.

Type
Session 3: Diagnostics of High Gravity Objects with X- and Gamma Rays
Information
Symposium - International Astronomical Union , Volume 188: The Hot Universe , 1998 , pp. 400 - 401
Copyright
Copyright © Kluwer 1998 

References

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