Light variations of the dwarf nova DX Andromedae during 10 consecutive orbital cycles

Details Light variations of the dwarf nova DX Andromedae during 10 consecutive orbital cycles Light variations of the dwarf nova DX Andromedae during 10 consecutive orbital cycles

Apr 1995

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995mnras.273..675h&link_type=abstract

Monthly Notices of the Royal Astronomical Society, Volume 273, Issue 3, pp. 675-680.

Astronomy and Astrophysics

Astronomy

6

Binaries: Close, Stars: Individual: Dx And, Novae, Cataclysmic Variables

Scientific paper

A total of 360 R-band and 76 I-band photometric observations of the long-period dwarf nova DX And is presented. All the data were obtained on five consecutive nights with a CCD camera on the 0.9-m James Gregory Telescope at the University Observatory, St Andrews, and provide the first detailed description of the light variations of DX And on orbital time-scales. It is shown that the light variations over the 10.6-h orbital period may be explained primarily by an ellipsoidal variation of amplitude 0.13 mag caused by synchronous rotation of the Roche-lobe-filling companion star, the dereddened (R-I) colour index of which corresponds to a spectral type of K0-1V. Additional variability, with a range of amplitude up to 0.05 mag, is also present at least in the R band and might itself exhibit the orbital period. This additional variability may be due to star-spot activity on the rapidly rotating and hence magnetically active K-type companion star, or to a variable contribution from a non-uniform accretion disc. Analysis of the light variations with the synthesis code LIGHT2 suggests an orbital inclination in the range 45 deg-53 deg, with a formal solution of 48 deg+/-1 deg for an adopted mass ratio of 0.9. Hence the overall model for the system proposed by Drew, Jones & Woods is well supported by these data, including the need for the companion to be oversized for its mass.

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