Phase resolved optical spectroscopy of the compact X-ray binary 2A1822-371

Details Phase resolved optical spectroscopy of the compact X-ray binary 2A1822-371 Phase resolved optical spectroscopy of the compact X-ray binary 2A1822-371

Sep 1982

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1982mnras.200..793m&link_type=abstract

Monthly Notices of the Royal Astronomical Society, vol. 200, Sept. 1982, p. 793-805.

Astronomy and Astrophysics

Astronomy

28

Binary Stars, Spectral Resolution, Stellar Spectrophotometry, Ultraviolet Spectra, Visible Spectrum, X Ray Sources, Absorption Spectra, Balmer Series, Ephemeris Time, Spectral Line Width, Stellar Color, Stellar Mass, Stellar Spectra, X Ray Spectra

Scientific paper

The optical, X-ray, and ultraviolet emissions of the X-ray system 2A1822-371 are modulated with a period of 5.57 hr. The 5.57 hr modulation is believed to reflect orbital motion about a mass donating companion star. The modulation at high energies is caused by the combined effects of an occultation by the companion and by a bulge on the accretion disk. The present investigation is concerned with an extension of the study of 2A1822-371, taking into account medium resolution optical spectroscopy of the system covering the 5.57 hr cycle. Broad shallow absorption lines are observed in the optical spectrum of 2A1822-371. These lines are similar to the rotationally broadened lines which are found in the spectra of disk accreting cataclysmic variables. Their presence in 2A1822-371 is, therefore, strong confirmation that it is a disk accreting star. The He II 4686 A and H-alpha emission lines have a breadth comparable to the absorption lines at all phases in the 5.57 hr cycle.

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