A Spectrophotometric Study of the Cataclysmic Variable 1329-294

Details A Spectrophotometric Study of the Cataclysmic Variable 1329-294 A Spectrophotometric Study of the Cataclysmic Variable 1329-294

Apr 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994mnras.267..957s&link_type=abstract

Monthly Notices of the Royal Astronomical Society, Vol. 267, NO. 4/APR15, P. 957, 1994

Astronomy and Astrophysics

Astronomy

10

Accretion, Accretion Discs - Binaries: Spectroscopic - Stars: Individual: 1329-294 - Novae, Cataclysmic Variables

Scientific paper

We present observations of the cataclysmic variable 1329-294. Spectrophotometry covering the region 3400-9600 Å reveals broad, double-peaked Balmer and He I emission, but no lines of high excitation. The continuum rises strongly into the red, but the red spectrum shows no secondary star features or ellipsoidal variations. The continuum and emission-line light curves display no eclipse structure and are dominated by flickering. An orbital period of 0.0748±0.0005d (107.7 min) is found from sinusoidal fits to the radial velocities of the emission lines. Folding of the data on this period yields a K-velocity of 132.6±4.2 km s-1 and a γ-velocity of 38.8±3.0 km s-1. Trailed spectra show a prominent S-wave within the emission lines, consistent with a bright-spot origin. Doppler tomography provides a successful test for the adopted orbital period and verifies the existence of the bright-spot. These maps indicate that there is little Balmer or He I emission from the secondary. The similarity between this system and many of the SU UMa-type dwarf novae encourages us to believe that we should place it in this category.

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