Orbital period of the dwarf nova HL Canis Majoris |
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| Authors: | M. D. Still,&dagger ,D. Steeghs,V. S. Dhillon, D. A. H. Buckley |
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| Affiliation: | NASA/Goddard Space Flight Center, Code 662, Greenbelt, MD 20771, USA; Physics and Astronomy, University of St Andrews, North Haugh, St Andrews, Fife KY16 9SS; Department of Physics and Astronomy, University of Sheffield, Sheffield S3 7RH; South African Astronomical Observatory, PO Box 9, Observatory 7935, Cape Town, South Africa |
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| Abstract: | We present a small sample of time-resolved optical spectroscopy of the dwarf nova HL CMa during an outburst state. By combining radial velocity measurements with published data we show that the previously quoted value is not the only candidate for the orbital period of this system. We reduce the significance of daily aliasing but cannot distinguish between two periods at 0.2146±0.0004 and 0.2212±0.0005 d. We show that the low-excitation emission lines are composites from an accretion disc and the companion star, and that high-excitation emission originates in the disc or outflowing material associated with the accreting white dwarf. |
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| Keywords: | accretion, accretion discs line: profiles binaries: close stars: individual: HL CMa novae: cataclysmic variables X-rays: stars |
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