Astronomy and Astrophysics – Astronomy
Scientific paper
Apr 1986
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986mnras.219..791h&link_type=abstract
Monthly Notices of the Royal Astronomical Society (ISSN 0035-8711), vol. 219, April 15, 1986, p. 791-808. SERC-supported researc
Astronomy and Astrophysics
Astronomy
84
Binary Stars, Dwarf Novae, Dynamic Models, Stellar Models, Stellar Spectra, White Dwarf Stars, Absorption Spectra, Accretion Disks, Balmer Series, Emission Spectra, High Resolution, Orbital Elements, Radial Velocity, Stellar Mass, Stellar Spectrophotometry
Scientific paper
Based on high-resolution phase resolved spectroscopy collected during June 1980 and April, May and June 1981 from the 2.5-m Mt Wilson reflector, a dynamical model of the dwarf nova binary AH Herculis is developed. A 600 km/s peak-to-peak separation is found for the distorted double-peaked Balmer emission lines from the accretion disk surrounding the white dwarf primary star. A 0.258116 + or - 0.000004 d binary period is determined based on emission line radial velocity variations over a one-year baseline. The weak absorption spectrum and orbital radial velocity curve of the cool mass-losing companion star AH Her B are measured, and its spectral type is found to be early-to-middle K with weaker Mg b lines than expected relative to Fe I. Imposing an empirical ZAMS mass-radius relationship on the companion star, the inclination is confined to 46 + or - 3 deg with component star masses of 0.95 + or - 0.10 solar masses for M(W), and 0.76 + or - 0.08 solar masses for M(R).
Horne Keith
Szkody Paula
Wade Richard A.
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