Phase-resolved spectroscopy of the novalike cataclysmic variable RW Sextantis

Details Phase-resolved spectroscopy of the novalike cataclysmic variable RW Sextantis Phase-resolved spectroscopy of the novalike cataclysmic variable RW Sextantis

Mar 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992a%26a...256..433b&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 256, no. 2, p. 433-437.

Astronomy and Astrophysics

Astrophysics

16

Accretion Disks, Astronomical Spectroscopy, Cataclysmic Variables, White Dwarf Stars, Balmer Series, Emission Spectra, H Beta Line, H Gamma Line, Stellar Magnitude, Stellar Mass Accretion

Scientific paper

From phase-resolved spectroscopy around H-beta and H-gamma we derive a secure orbital period of 0.24507(20) days. We report the discovery of narrow Balmer emission-line components from the heated hemisphere of the secondary facing the white dwarf. Combined with the Balmer absorption lines from the accretion disk, the system effectively becomes a double-lined spectroscopic binary. The mass ratio is q = M1/M2 = 1.35 +/- 0.10. The inclination is between i = 28 deg and about 40 deg and is not sufficiently constrained to derive accurate masses. The distance of RW Sex is d about 150 pc and its absolute magnitude M(v) about 4.8.

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