Optical emission-line formation by the high-temperature gas in X-ray sources

Details Optical emission-line formation by the high-temperature gas in X-ray sources Optical emission-line formation by the high-temperature gas in X-ray sources

Dec 1979

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1979sval....5..318b&link_type=abstract

(Pis'ma v Astronomicheskii Zhurnal, vol. 5, Nov. 1979, p. 595-600.) Soviet Astronomy Letters, vol. 5, Nov.-Dec. 1979, p. 318-321

Astronomy and Astrophysics

Astronomy

Astronomical Spectroscopy, High Temperature Plasmas, Interstellar Gas, Optical Emission Spectroscopy, X Ray Sources, Emission Spectra, Flare Stars, Hydrogen Ions, Line Spectra

Scientific paper

Emission spectra are calculated for gas optically thin with respect to free-free absorption and heated to 10-million K. Lines of hydrogen and hydrogen-like ions might be detectable if the optical depth for Thomson scattering is tau(T) in the range 3-10. The positions of these expected lines are compared with the features in the optical spectrum of the transient X-ray source A0620-00. During the period of observation the emission lines may possibly have been formed in a hot gas cloud, optically thin to free-free absorption, and responsible for the soft X-rays as well.

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