Computer Science – Numerical Analysis
Scientific paper
Nov 1994
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994apj...435l.129k&link_type=abstract
Astrophysical Journal, Part 2 - Letters (ISSN 0004-637X), vol. 435, no. 2, p. L129-L132
Computer Science
Numerical Analysis
22
Accretion Disks, Black Holes (Astronomy), Dynamo Theory, Gravitational Effects, Magnetohydrodynamics, Stellar Magnetic Fields, Stellar Rotation, Computerized Simulation, Magnetic Effects, Numerical Analysis, Plasma Oscillations, Poloidal Flux, Relativity
Scientific paper
We present a previously unknown dynamo effect that arises from the coupling of the gravitomagnetic field of a Kerr black hole with electromagnetic fields. The axisymmetric dynamo equations are derived in the 3 + 1 split of Kerr spacetime. They are formally identical to their equivalents in flat space, augmented by a general relativistic source term for the poloidal magnetic field provided by the gravitomagnetic field. There is no need for any particular small-scale plasma motions. The effect does, however, require finite conductivity and is enhanced by anomalous or turbulent magnetic diffusivity. The results of our time-dependent numerical simulations of the mean field dyanmo in a turbulent accretion disk prove that the gravitomagnetic dynamo has growing modes in the vicinity of a rotating black hole.
Camenzind Max
Khanna Ramon
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