Astronomy and Astrophysics – Astrophysics
Scientific paper
Aug 1994
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994a%26a...288..204b&link_type=abstract
Astronomy and Astrophysics (ISSN 0004-6361), vol. 288, no. 1, p. 204-212
Astronomy and Astrophysics
Astrophysics
27
Balmer Series, Cataclysmic Variables, Eclipsing Binary Stars, Light Curve, Stellar Mass, Stellar Orbits, X Ray Spectra, Emission Spectra, H Alpha Line, H Beta Line, Helium, Orbital Elements, Spectrum Analysis, Stellar Spectrophotometry
Scientific paper
We present high-speed UBVR - photometry and time-resolved spectroscopy of the X-ray source 1H 1752+081. The light curves are characterized by a double eclipse repeating at the orbital period of 112.97 min. and an orbital hump occurring between eclipse phases phi approximately = 0.50 and phi approximately = 0.85. The spectra show strong Balmer lines and the lines of HeI and HeII in emission. The line profiles are characterized by a time-variable broad base component and superposed to them (best seen in Halpha and Hbeta) a narrow component whose variation is phase-shifted with respect to the base component. Our observations are consistent with 1H 1752+081 being a cataclysmic binary of the AM Her subtype observed in a high state. Eclipse analysis and measurement of the radial velocity amplitude of the narrow component of Halpha allow estimating the physical parameters. The mass of the white dwarf is M1 approximately = (0.9 +/- 0.1) solar mass, the best estimate of the secondary mass M2 approximately = 0.185 solar mass, but values in the range 0.1 solar mass. M2. 0.25 solar mass cannot be ruled out. The parameters are consistent with what one expects from theory for an AM Her star close to the 114 min. period spike, i.e. with the secondary being close to the main sequence and M1 greater than or = 0.7 solar mass.
Barnbantner O.
Barwig Heinz
Ritter Hans
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