Time-resolved ultraviolet spectroscopy of the cataclysmic variable, PG 1711 + 336

Details Time-resolved ultraviolet spectroscopy of the cataclysmic variable, PG 1711 + 336 Time-resolved ultraviolet spectroscopy of the cataclysmic variable, PG 1711 + 336

Jan 1991

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991mnras.248...40p&link_type=abstract

Monthly Notices of the Royal Astronomical Society (ISSN 0035-8711), vol. 248, Jan. 1, 1991, p. 40-47. Research supported by SERC

Astronomy and Astrophysics

Astronomy

7

Cataclysmic Variables, Stellar Spectra, Stellar Winds, Ultraviolet Spectroscopy, Iue, Line Spectra, Resonance Lines, Stellar Models

Scientific paper

Low-resolution IUE ultraviolet observations of the cataclysmic variable, PG 1711 + 336, are presented. The spectra reveal extensive variability in the wind-formed C IV 1550 A resonance line P Cygni profiles, on time-scales as short as several hours. The high-resolution IUE spectrum of the nova-like system V3885 Sgr, convolved with the IUE low-resolution instrumental profile, provides a good match to the low-resolution wind lines of PG 1711 + 336 at some epochs. Hot-star wind theory and spherical symmetry are assumed in order to model the high-resolution data. The results yield a crude time-independent (lower-limit) estimate for the product of mass-loss rate and ion fraction. Moments of the observed P Cygni profiles in PG 1711 + 336 are measured to quantify the wind variability, and suggest that the C IV wind column densities may vary by a factor of about 2 in about 1 hour. Changes of a factor of about 2 in the edge velocities of the shortward-shifted resonance lines, with maximum values about 4500 km/s, are calculated.

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