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Three-Dimensional Global MHD Simulations of Magnetised Accretion Disks and Jets

Published online by Cambridge University Press:  12 April 2016

R. Matsumoto  and
K. Shibata
R. Matsumoto*
Affiliation:
Department of Physics, Faculty of Science, Chiba University, 1–33 Yayoi-Cho, Inage-ku, Chiba 263, JAPAN
K. Shibata
Affiliation:
National Astronomical Observatory, Mitaka, Tokyo 181, JAPAN
*
1Advanced Science Research Center, JAERI, Naka, Japan

Abstract

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We carried out three-dimensional global MHD simulations of jet formation from an accretion disk threaded by large-scale magnetic fields. Numerical results show that bipolar jets with maximum speed υjet ~ υKepler are created. The surface layer of the disk accretes faster than the equatorial part because magnetic braking most effectively affects that layer. Accretion proceeds along spiral channels which correspond to the surface avalanche flow appearing in previous axisymmetric simulations. Spirally shaped low β (= Pgas/Pmag < 1) regions appear in the innermost part of accretion disks where toroidal magnetic fields become dominant.

Type
Part 10. Accretion Disks and Outflows
Information
International Astronomical Union Colloquium , Volume 163: Accretion Phenomena and Related Outflows , 1997 , pp. 443 - 447
Copyright
Copyright © Astronomical Society of the Pacific 1997

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