Geodesic synchrotron radiation in the Kerr geometry by the method of asymptotically factorized Green's functions

Details Geodesic synchrotron radiation in the Kerr geometry by the method of asymptotically factorized Green's functions Geodesic synchrotron radiation in the Kerr geometry by the method of asymptotically factorized Green's functions

Sep 1974

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1974phrvd..10.1701c&link_type=abstract

Physical Review D - Particles and Fields, 3rd Series, vol. 10, Sept. 15, 1974, p. 1701-1721. Research supported by the Science R

Astronomy and Astrophysics

Astronomy

26

Black Holes (Astronomy), Green'S Functions, Relativistic Particles, Synchrotron Radiation, Asymptotic Methods, Circular Orbits, Gravitational Fields, Kerr Effects, Radiation Spectra, Wave Equations

Scientific paper

The scalar, electromagnetic, and gravitational geodesic-synchrotron-radiation (GSR) spectra are determined for the case of a test particle moving on a highly relativistic circular orbit about a rotating (Kerr) black hole. It is found that the spectral shape depends only weakly on the value of the angular-momentum parameter (a/M) of the black hole, but the total radiated power drops unexpectedly for a value of at least 0.95 and vanishes as the value approaches unity. A spin-dependent factor (involving the inner product of the polarization of a radiated quantum with the source) is isolated to explain the dependence of the spectral shape on the spin of the radiated field. Although the scalar wave equation is solved by separation of variables, this procedure is avoided for the vector and tensor cases by postulating a sum-over-states expansion for the Green's function similar to that found to hold in the scalar case. The terms in this sum, significant for GSR, can then be evaluated in the geometric-optics approximation without requiring the use of vector or tensor spherical harmonics.

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