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Effects of magnetic field on the runaway instability of relativistic accretion tori near a rotating black hole

Published online by Cambridge University Press:  22 May 2014

V. Karas  and
J. Hamerský
V. Karas
Affiliation:
Astronomical Institute, Academy of Sciences, Prague, Czech Republic email: vladimir.karas@cuni.cz
J. Hamerský
Affiliation:
Astronomical Institute, Academy of Sciences, Prague, Czech Republic email: vladimir.karas@cuni.cz
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Abstract

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Runaway instability operates in accretion tori around black holes, where it affects systems close to the critical (cusp overflowing) configuration. The runaway effect depends on the radial profile l(R) of the angular momentum distribution of the fluid, on the dimension-less spin a of the central black hole (|a| ≤ 1), and other factors, such as self-gravity. Here we discuss the role of runaway instability within a framework of an axially symmetric model of perfect fluid endowed with a purely toroidal magnetic field.

Keywords

Accretionaccretion disks – gravitation – black hole physics
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 9 , Symposium S303: The Galactic Center: Feeding and Feedback in a Normal Galactic Nucleus , October 2013 , pp. 424 - 426
Copyright
Copyright © International Astronomical Union 2014 

References

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