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Astron. Astrophys. 351, 1021-1027 (1999)

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

J.E. Steiner 1,2, D. Cieslinski 3, F.J. Jablonski 3 and R.E. Williams 4

1 Laboratório Nacional de Astrofísica/CNPq, CP 21, 37500-000 Itajubá, Brazil
2 Instituto Astronômico e Geofísico, Universidade de São Paulo, CP 9638, 01065-970 São Paulo, Brazil
3 Divisão de Astrofísica, Instituto Nacional de Pesquisas Espaciais, CP 515, 12201-970 São José dos Campos, Brazil
4 Space Telescope Science Institute-STScI, 3700 San Martin Drive, Baltimore, MD 21218, USA

Received 11 June 1999 / Accepted 15 September 1999


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. H[FORMULA] 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.

Key words: stars: novae, cataclysmic variables – stars: individual: V617 Sgr – stars: binaries: eclipsing – stars: Wolf-Rayet – X-rays: stars

* Based on observations made at Laboratório Nacional de Astrofísica/CNPq, Brazil, and Cerro Tololo Interamerican Observatory-CTIO, Chile.

Send offprint requests to: J.E. Steiner (steiner@lna.br)

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© European Southern Observatory (ESO) 1999

Online publication: November 16, 1999