Ultraviolet studies of nova-like variables with the IUE

Details Ultraviolet studies of nova-like variables with the IUE Ultraviolet studies of nova-like variables with the IUE

Sep 1983

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1983stin...8417080g&link_type=abstract

Final Report, Apr. 1981 - Sep. 1983 Villanova Univ., PA. Dept. of Astronomy.

Astronomy and Astrophysics

Astronomy

Accretion Disks, Balmer Series, Steady State, Variable Stars, Binary Systems (Materials), Dwarf Novae, Gas Flow, Iue, Phase Modulation, Red Shift, Ultraviolet Astronomy

Scientific paper

KQ Mon is a new UX UMa-type nova-like variable. Optical spectra taken in 1978 reveal very shallow Balmer absorption lines and He I (wavelength 4471) absorption. There was no evidence of orbital variations but the appearance of the optical spectrum and the presence of low amplitude flickering suggested a strong similarity to CD-42 degrees 14462 (=V3885 Sgr) and other members of the UX UMa class. KQ Mon was observed at low dispersion with the IUE satellite. Six spectra taken with the short wavelength prime (SWP) camera are dominated by strong broad absorption lines due to N V, O I, Si III, Si IV, C IV, He II, N IV, and A1 III. There is little evidence of orbital phase modulation over the time baseline of the observations. Unlike UV observations of other UX UMa-type objects, KQ Mon exhibits no emission lines or P Cygni-type profiles and the velocity displacements appear to be smaller, suggesting the absence of a hot, high velocity wind characterizing other UX UMa stars. The relationship of KQ Mon to other UX UMa disk stars is discussed and a model is suggested to explain their observed properties and the lack of major outbursts.

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