Abstract
We present the results obtained from unfiltered photometric CCD observations of V1193 Ori made during 24 nights between November 2002 and January 2003. We found periods of 0.1430 d , 0.1362 d and possibly 2.98 d in the data. The 0.1430 d period is consistent with the 1 d −1 alias of the proposed orbital period of P orb = 0.165 d (Ringwald, F.A., Thorstensen, J.R., Hamwey, R.M., 1994. MNRAS 271, 323; Papadaki, C., Boffin, H.M.J., Cuypers, J., Stanishev, V., Kraicheva, Z., Genkov, V., 2004. In: Hilditch, R.W., Hensberge, H., Pavlovski, K. (Eds.), Spectroscopically and Spatially Resolving the Components of Close Binary Stars, ASP Conference Series, vol. 318, Astronomical Society of the Pacific, San Francisco, p. 399.). Thus and using the known relation between the orbital and superhump periods, we interpret these periods as the orbital period of 0.1430 d , the negative superhump period of 0.1362 d and the precession period of 2.98 d . V1193 Ori can then be classified as a permanent superhump system.
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