Orbital period of the dwarf nova HL Canis Majoris

Details Orbital period of the dwarf nova HL Canis Majoris Orbital period of the dwarf nova HL Canis Majoris

Nov 1999

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999mnras.310...39s&link_type=abstract

Monthly Notices, Volume 310, Issue 1, pp. 39-42.

Astronomy and Astrophysics

Astronomy

2

Accretion, Accretion Discs, Line: Profiles, Binaries: Close, Stars: Individual: Hl Cma, Novae: Cataclysmic Variables, X-Rays: Stars

Scientific paper

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+/-0.0005d. 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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