Formation of Balmer lines in the spectra of x-ray novae

Details Formation of Balmer lines in the spectra of x-ray novae Formation of Balmer lines in the spectra of x-ray novae

Jan 1998

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1998astl...24...22s&link_type=abstract

Astronomy Letters, Volume 24, Issue 1, January 1998, pp.22-33; Pis'ma v Astronomicheskii Zhurnal, Vol. 24, p. 26

Astronomy and Astrophysics

Astronomy

2

Scientific paper

The profiles and equivalent widths of the absorption and emission components of Balmer lines and the continuum optical spectra of X-ray novae during outbursts are calculated. A stationary self-illuminated accretion alpha disk around a Schwarzschild black hole is used as an instantaneous model for the X-ray nova. Each annulus of the disk is assumed to emit as a stellar atmosphere that is illuminated by the same X-ray flux. The irradiated stellar model atmospheres are calculated in the LTE approximation. The equivalent widths of the emission components of the Balmer lines are shown to depend on the X-ray flux that is intercepted by the disk (i.e., on the geometric sizes of the disk), on the optical depth of the chromospheric-like layer along the line of sight (i.e., on the inclination of the disk to the line of sight), and on the relative fraction of the soft component with E ~ 0.1 keV in the X-ray spectrum (because it is this component that heats the upper atmosphere of the disk). A comparison of the theoretical spectra with the observed spectra of the X-ray nova V518 Per (GROJ0422+32) reveals an additional emission in the observed spectrum, which is most probably the bremsstrahlung of an optically thin, hot (T ~ 10^6 K) shell.

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