Astronomy and Astrophysics – Astrophysics
Scientific paper
Feb 1994
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994a%26a...282..493r&link_type=abstract
Astronomy and Astrophysics (ISSN 0004-6361), vol. 282, no. 2, p. 493-502
Astronomy and Astrophysics
Astrophysics
29
Balmer Series, Cataclysmic Variables, Emission Spectra, Optical Emission Spectroscopy, Orbital Elements, Stellar Mass Accretion, Ultraviolet Spectra, White Dwarf Stars, Absorption Spectra, Charge Coupled Devices, K Stars, Light Curve, Mass Ratios, Polar Regions, Radial Velocity, Spectral Resolution, Stellar Luminosity, Telescopes
Scientific paper
We present spin-phase resolved spectroscopy of the nova-like cataclysmic variable (CV) AE Aquarii. Unlike in other magnetic CVs, the pulsed fraction of the Balmer emission line intensities is small and must be below the detection limit of approximately 2%. From the absorption lines of the K star secondary we derive an improved orbital ephemeris which is 180 deg out of phase with respect to the pulse-timing orbit of Robinson et al. (1990, 1991). Combining their pulse-timing amplitude with the absorption line radial velocity amplitude, we find the mass ratio q = M2/M1 = (0.77 +/- 0.03). The most probably masses of the binary components are M1 = 0.91 solar mass and M2 = 0.70 solar mass giving an inclination i = 57 deg. During optical flares, a complex structure with rapid velocity variations has been observed in the Balmer emission lines which could originate from the accretion flow towards the magnetic polar regions of the white dwarf.
Beuermann Klaus
Reinsch Klaus
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