WX Cen and the nature of the V Sagittae stars

Details WX Cen and the nature of the V Sagittae stars WX Cen and the nature of the V Sagittae stars

Aug 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003basbr..23..135s&link_type=abstract

Boletim da Sociedade Astronômica Brasileira (ISSN 0101-3440), vol.23, no.1, p. 135-135

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Scientific paper

WX Cen is one of the 4 V Sagittae stars known up to now, besides V Sge, V617 Sgr and DI Cru. The objects of this class are binary systems characterized by strong emission lines of O VI and N V, and by the ratio He II 4686Å/Hb > 2. We performed CCD photometry and Cassegrain spectroscopy on March and April 2000 at LNA. We also obtained a FEROS spectrum on January 2002 at the ESO 1,5m telescope. We confirmed the orbital period as being 10 hours, in agreement with Diaz and Steiner (1995). The light curve has an amplitude of ~0.32 mag and has a narrow minimum, similar to the ones seen in V Sge and V617 Sgr. The spectra show highly variable satellites in the Balmer lines in absorption with v = -2900 km/s and in emission with v = +/- 3500 km/s. An analysis of the He II Pickering series decrement shows that the system has significant amount of Hydrogen. Interstellar absorption in Na ID and Ca II show components at v = -4.1km/s, which corresponds to the velocity of the Coal sack, and three other components at v = -23.9, -32.0 and -39.0 km/s. These components are also seen with similar strengths in field stars that have distances between 1.8 and 2.7 kpc. We have detected nebular emission in [S II], [N II] and Ha. The object presents redshifted emission in high ionization species. The O VI lines show strong variability with velocity of about 750 to 800 km/s. One possible explanation may be obtained by a comparison with V617 Sgr. Depending on the phase, an elevated rim at the border of the accretion disk, produced by the accretion flow, would produce the red peaks seen in the lines. Besides, a spill-over stream could explain the high red velocities. An alternative model would be that the white dwarf is highly magnetized, producing gravitational redshift in high ionization species and high velocity inflow, always seen in the red, with high degree of variability.

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