Optical spectroscopy of the X-ray transient GS 2023 + 338 (= V404 Cygni)

Details Optical spectroscopy of the X-ray transient GS 2023 + 338 (= V404 Cygni) Optical spectroscopy of the X-ray transient GS 2023 + 338 (= V404 Cygni)

Jan 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992aj....103..219g&link_type=abstract

Astronomical Journal (ISSN 0004-6256), vol. 103, Jan. 1992, p. 219-228.

Astronomy and Astrophysics

Astronomy

8

Accretion Disks, Astronomical Spectroscopy, Novae, X Ray Sources, Distance, Emission Spectra, Interstellar Extinction, Line Spectra

Scientific paper

The paper presents spectroscopic observations of V404 Cygni obtained during the decline from a major outburst. The spectral evolution over the period from July 1989 to May 1990 is followed, and a spectrum characteristic of emission from an accretion disk in a close binary system is found. V404 Cyg displays a smooth continuum, lacking in stellar absorption features, with broad, double-peaked Balmer, He, and Fe emission lines whose velocity widths (FWHM about 600-1400 km/s) increased with time. The increasing line widths are interpreted as evidence for a decrease in the outer radius of the disk's emission-line region. Time-resolved spectroscopy sets an upper limit on the semiamplitude of the projected velocity variation of the compact object of K1 less than about 25 km/s, for orbital periods less than 6 hr. A classical mass determination is not possible, but, if the emission lines originate in the outer disk, as their profiles suggest, then, for the most likely range of the orbital period (4-6 hr), the binary inclination i is less than about 20 deg, and the mass of the compact star is greater than about 1.4 solar mass.

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