Relativistic Magnetic Reconnection in Kerr Spacetime
Asenjo
F
A
author
Comisso
L
author
2017
English
The magnetic reconnection process is analyzed for relativistic magnetohydrodynamical plasmas around rotating black holes. A simple generalization of the Sweet-Parker model is used as a first approximation to the problem. The reconnection rate, as well as other important properties of the reconnection layer, has been calculated taking into account the effect of spacetime curvature. Azimuthal and radial current sheet configurations in the equatorial plane of the black hole have been studied, and the case of small black hole rotation rate has been analyzed. For the azimuthal configuration, it is found that the black hole rotation decreases the reconnection rate. On the other hand, in the radial configuration, it is the gravitational force created by the black hole mass that decreases the reconnection rate. These results establish a fundamental interaction between gravity and magnetic reconnection in astrophysical contexts.
WOS:000396415100005
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text
files/702_Asenjo+Comisso2017.pdf
10.1103/PhysRevLett.118.055101
Asenjo+Comisso2017
Physical Review Letters
Phys. Rev. Lett.
2017
Amer Physical Soc
continuing
periodical
academic journal
118
5
5 pp
0031-9007