The photometric and spectroscopic characterization of the V Sagittae star V617 Sagittarii

Details The photometric and spectroscopic characterization of the V Sagittae star V617 Sagittarii The photometric and spectroscopic characterization of the V Sagittae star V617 Sagittarii

Nov 1999

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999a%26a...351.1021s&link_type=abstract

Astronomy and Astrophysics, v.351, p.1021-1027 (1999)

Astronomy and Astrophysics

Astrophysics

12

Stars: Novae, Cataclysmic Variables, Stars: Individual: V617 Sgr, Stars: Binaries: Eclipsing, Stars: Wolf-Rayet, X-Rays: Stars

Scientific paper

Photometric and spectroscopic characterization of the V Sge star V617 Sgr (WR 109) is presented. The orbital period, 0.207 day, is the shortest of its class. The optical light curve presents a double wave with minima and maxima of uneven brightness. Strong emission lines of highly ionized species such as HeII, NV and OVI dominate the optical spectrum. High and low photometric states have been observed and the primary eclipse becomes shallower at eruptions. Hα emission becomes stronger and broader at high state when compared to low state. The striking similarities to V Sge are discussed. The photometric and spectroscopic observations suggest that a high and asymmetric rim exists associated with the accretion disk. This star is interpreted as a X-ray quiet galactic counterpart of the supersoft X-ray binaries seen in the Magellanic Clouds. Based on observations made at Laboratório Nacional de Astrofísica/CNPq, Brazil, and Cerro Tololo Interamerican Observatory--CTIO, Chile.

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