Spectroscopic observations of the detached binary PG 1413 + 015

Details Spectroscopic observations of the detached binary PG 1413 + 015 Spectroscopic observations of the detached binary PG 1413 + 015

Mar 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993apj...406..240f&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 406, no. 1, p. 240-246.

Astronomy and Astrophysics

Astrophysics

23

Eclipsing Binary Stars, Stellar Atmospheres, Stellar Mass, Stellar Temperature, White Dwarf Stars, Balmer Series, Cataclysmic Variables, Light Curve, Ultraviolet Spectra

Scientific paper

We present improved estimates of the stellar parameters of the eclipsing, precataclysmic binary system PG 1413 + 015 (GH Vir), which has an orbital period of only 8h16m. Model atmosphere fits a Balmer line profiles yield T(eff) = 48,800 +/- 1200 K and log g = 7.70 +/- 0.11 for the DAO white dwarf primary star, from which a mass of 0.51 +/- 0.04 solar mass is inferred using evolutionary models. An ultraviolet spectrum obtained with the IUE Observatory has a slope consistent with this temperature and the assumption of no interstellar extinction. A red CCD spectrum of the secondary star during the 12-minute total eclipse indicates a spectral type of M3 V-M5 V. Reanalysis of the eclipse light curve leads to an inferred radius of 0.15 solar radius and a mass of 0.10 solar mass for the secondary, the latter being marginally consistent with the spectral type. Reprocessing on the facing side of the secondary produces phase-dependent Balmer line emission and detectable variations in the continuum from 6500-9000 A. The observed levels of reprocessing are consistent with expectations based on the above stellar parameters.

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