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Steady models of optically thin, magnetically supported two-temperature accretion disks around a black hole

Published online by Cambridge University Press:  01 August 2006

H. Oda ,
K. E. Nakamura ,
M. Machida  and
R. Matsumoto
H. Oda
Affiliation:
Graduate School of Science and Technology, Chiba University, 1-33 Yayoi-Cho, Inage-ku, Chiba 263-8522, Japan email: oda@astro.s.chiba-u.ac.jp
K. E. Nakamura
Affiliation:
Department of Sciences, Matsue National College of Technology, 14-4 Nishiikuma-Cho, Matsue, Shimane 690-8518, Japannakamrkn@matsue-ct.jp
M. Machida
Affiliation:
Division of Theoretical Astronomy, National Astronomical Observatory ofJapan, 2-21-1 Osawa, Mitaka, Tokyo 181-8588, Japanmami@th.nao.ac.jp
R. Matsumoto
Affiliation:
Department of Physics, Faculty of Science, Chiba University, 1-33 Yayoi-Cho, Inage-ku, Chiba 263-8522, Japanmatumoto@astro.s.chiba-u.ac.jp
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Abstract

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We obtained steady solutions of optically thin two-temperature magnetized accretion disks around a black hole. We included relativistic bremsstrahlung cooling, synchrotron cooling and inverse Compton effects and assumed that the disk is threaded by toroidal magnetic field. We found that a magnetic pressure dominated new branch, which we call a ‘low-β branch’, appears in the thermal equilibrium curves. The luminosity of the optically thin, magnetically supported disk can exceed 10% of the Eddington luminosity (0.1 LEdd).

Keywords

Accretion: accretion disks – black holes – state transitions – MHD
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 2 , Symposium S238: Black Holes from Stars to Galaxies – Across the Range of Masses , August 2006 , pp. 421 - 422
Copyright
Copyright © International Astronomical Union 2007

References

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