The stellar mass ratio of GK Persei |
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| Authors: | L Morales-Rueda MD Still P Roche JH Wood JJ Lockley |
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| Institution: | 1Department of Physics and Astronomy, University of Southampton, Highfield, Southampton SO17 1BJ;2NASA Goddard Space Flight Center, Code 662, Greenbelt, MD 20771, USA;3Universities Space Research Association, 7501 Forbes Blvd, Suite 206, Seabrook, MD 20706, USA;4Physics and Astronomy, University of St Andrews, North Haugh, St Andrews, Fife KY16 9SS;5Department of Physics and Astronomy, University of Leicester, University Road, Leicester LE1 7RH;6School of Chemistry and Physics, Keele University, Keele, Staffordshire ST5 5BG;7Department of Astronomy, San Diego State University, San Diego, CA 92182, USA |
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| Abstract: | We study the absorption lines present in the spectra of the long-period cataclysmic variable GK Per during its quiescent state, which are associated with the secondary star. By comparing quiescent data with outburst spectra we infer that the donor star appears identical during the two states and the inner face of the secondary star is not noticeably irradiated by flux from the accreting regions. We obtain new values for the radial velocity semi-amplitude of the secondary star,  , a projected rotational velocity,  and consequently a measurement of the stellar mass ratio of GK Per,  . The inferred white dwarf radial velocities are greater than those measured traditionally using the wings of Doppler-broadened emission lines suspected to originate in an accretion disc, highlighting the unsuitability of emission lines for mass determinations in cataclysmic variables. We determine mass limits for both components in the binary,  and  . |
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| Keywords: | binaries: close stars: fundamental parameters stars: individual: GK Per novae cataclysmic variables |
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