The profile evolution of X-ray spectral lines due to Comptonization - Monte Carlo computations

Details The profile evolution of X-ray spectral lines due to Comptonization - Monte Carlo computations The profile evolution of X-ray spectral lines due to Comptonization - Monte Carlo computations

May 1979

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1979a%26a....75..214p&link_type=abstract

Astronomy and Astrophysics, vol. 75, no. 1-2, May 1979, p. 214-222.

Astronomy and Astrophysics

Astrophysics

43

Compton Effect, Computerized Simulation, Monte Carlo Method, Plasma Clouds, Thomson Scattering, X Ray Spectra, Electron Energy, Galactic Nuclei, Line Spectra, Optical Thickness, Radiative Transfer, Silicon

Scientific paper

The profile evolution of iron X-ray lines due to multiple Compton scattering in a plasma cloud with Thomson optical depths of 1 to 10 at various electron temperatures is examined. The profile of the once-scattered Kalpha line is analyzed for two special cases: negligible Doppler effect (electron temperature = zero) and negligible recoil effect (photon energies much greater than electron temperature). The formulas and weighted Monte Carlo techniques reported in a previous paper by the authors (1977) are used to compute the spectra of the Ly alpha silicon line (photon energy = 2 keV) emerging from plasma clouds with an electron temperature of 10 keV and Thomson optical depths of 3, 5, 10 and 20. Power-law tails with a slope weakly dependent on the spectrum of initial photons are found to arise in a broad energy band. These tails resemble those observed in Cyg X-1 and some nuclei of galaxies and quasars.

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