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Author Chou, W. ♦ Tajima, T.
Source United States Department of Energy Office of Scientific and Technical Information
Content type Text
Language English
Subject Keyword PHYSICS ♦ SCHWARZSCHILD METRIC ♦ PLASMA INSTABILITY ♦ BLACK HOLES ♦ SCHWARZSCHILD RADIUS ♦ RELATIVISTIC PLASMA ♦ CONVECTIVE INSTABILITIES ♦ MAGNETIC FIELDS ♦ ACCRETION DISKS ♦ HYDRODYNAMICS ♦ MAGNETOHYDRODYNAMICS
Abstract General relativistic plasma dynamics relevant to the condition very close to a black hole event horizon is developed. The plasma is studied using the 3{plus}1 paradigm of general relativistic magnetohydrodynamics. The equilibrium and dynamical solution of such a plasma in Rindler{close_quote}s coordinates are presented. We assume a pressure source at the horizon that provides the balancing force to stop the radial infall of the plasma. We show that the plasma near the black hole is subject to the convective instability when the magnetic field is absent and to the magnetic buoyancy instability when a toroidal field exists. These instabilities are largely suppressed, however, in the presence of a poloidal magnetic field. Therefore, when a poloidal magnetic field is twisted and changed into a toroidal field by plasma rotation, the plasma is destabilized due to these instabilities. The manifestation of these instabilities is a jet formation from this inner region of a black hole atmosphere. Since this formation mechanism is deep in the gravitational potential of a black hole, the energy liberated and the jet formed by this mechanism can be very substantial. We suggest that this mechanism provides a viable model for recent observations of the superluminal jets from the galactic black hole candidates GRS 1915{plus}105 and GRO J1655{minus}40. {copyright} {ital {copyright} 1999.} {ital The American Astronomical Society}
ISSN 0004637X
Educational Use Research
Learning Resource Type Article
Publisher Date 1999-03-01
Publisher Place United States
Journal Astrophysical Journal
Volume Number 513
Issue Number 1


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