On the radiation emitted by a particle falling into a black hole in the semirelativistic approximation

Details On the radiation emitted by a particle falling into a black hole in the semirelativistic approximation On the radiation emitted by a particle falling into a black hole in the semirelativistic approximation

Dec 1985

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985stin...8711664c&link_type=abstract

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Astronomy and Astrophysics

Astronomy

Black Holes (Astronomy), Electromagnetic Radiation, Relativistic Particles, Relativistic Theory, Coordinates, Maxwell Equation, Particle Energy, Relativity

Scientific paper

The semirelativistic approximation is used to compute the electromagnetic energy emitted when a charged particle falls into a Reissner-Nordstrom black hole. Results are compared with those obtained by integrating numerically the perturbed Maxwell equations in the case of radial fall. The semirelativistic approximation method requires much less computer time, because part of the calculations can be done analytically, and it can be applied to any given geodesic followed by the particle. It is shown that in the case of spherically symmetric black holes the approximate method gives realistic results: it predicts the correct behavior of the radiation versus the angular momentum of the particle and the correct order of magnitude of the amount of energy emitted. When the method is applied to rotating black holes the use of the Boyer-Lindquist coordinates is forbidden by the effects of the infinite rotation of the particle when it approaches the radius of the horizon. It is shown that different choices of the coordinate systems give different results.

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