CBA Center for Backyard Astrophysics

Superhumps in Cataclysmic Binaries. XIV. V592 Cassiopeiae

Cynthia Taylor, John Thorstensen, Robert Fried, Joseph Patterson, Tonny Vanmunster, David Harvey, David Skillman, Lasse Jensen, and Sergei Shugarov

Publications of the Astronomical Society of the Pacific

October 1998, Volume 110, Page 1148

We report a spectroscopic and photometric study of the novalike variable V592 Cassiopeiae (= LS I 55°-8). The spectrum is that of a typical UX Ursae Majoris star, with weak, narrow Balmer emission superposed on broad absorption. The emission lines move with P = 0.115063(1) d, which is presumably the underlying orbital period of the binary. Photometry reveals a different period, namely 0.12228(1) d. The presence of this wave in a short-period cataclysmic variable, and the value of the period excess at 6.3%, suggests identification as a "permanent superhump". After subtraction of this large signal, the residual time series appears to contain a weak feature at 0.11193(5) d. The star evidently shows positive and negative superhumps simultaneously.



Copyright © 1998 Astronomical Society of the Pacific.