Compton Backscattering as a Thermometer for Cosmic Plasmas

Astronomy and Astrophysics – Astronomy

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As distinct from the classical Compton scattering of photons off cold, non-relativistic electron gas, the differential Klein-Nishina cross-section of the Compton effect for electrons with relativistic bulk motion reaches its maximum value at the scattering angle theta = 180(deg) , i.e. in the opposite direction relative to that of incident photons. We consider the effect of backscattering in the case when electrons, in addition to bulk motion, have a Maxwellian distribution in velocities. It is shown that, in this case, the maximum is essentially weakened at temperatures exceeding ~ 1 KeV, basically as a result of just one Compton scattering. The location and the value of the maximum are very sensitive to the electron temperature of the scattering plasma. Therefore, the Compton backscattering might serve as a fine tool to measure the plasma temperature at the sites where the backscattering features are formed. The shape of the continuum emission contains important information on geometry, including the location of the 511 KeV line source relative to the accretion disk(1) . Assuming that the main reflection target is the accretion disk atmosphere, we discuss the mass determination issue for the underlying sources. Some implications of the elaborated theory for cosmic sources of the 511 KeV line, including black-hole candidates, are presented. For those candidates whose spectra contain, besides the 511 KeV line, a softer (1 -- 10 KeV) X-ray component, there is an opportunity to compare the derived mass of the source with that derived by an alternative method that employs our techniques elaborated for electron scattering atmospheres(2) . (1) Lingenfelter, R.E. and Hua, X.-M. 1991, Ap. J. 381, 426 (2) Ebisawa, K., Titarchuk, L.G., Ozernoy, L., White, N.E., and Mitsuda, K. This meeting () NAS/NRC Senior Research Associate

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