2005/06/21 by A. Olech, K. Zloczewski, Olech, A. +9
Physics and Astronomy · #Astrophysics (astro-ph) #FOS: Physical sciences #astro-ph
paper · pdf · doi:10.48550/arxiv.astro-ph/0506487
11 pages, 7 figures, Acta Astronomica, in print
arxiv created 2005/06/21 · arxiv updated 2009/12/01
We report extensive photometry of the dwarf nova V660 Herculis. During our campaign, lasting from August 2003 to November 2004, we recorded one bright eruption which turned out to be a superoutburst lasting about 15 days and having amplitude of ~4.5 mag. Clear superhumps with a mean period of Psh = 0.080924(18) days were present during all nights of the superoutburst. The period of the superhumps was not stable and in the interval covered by our observations it decreased with a rate of -4.0(1.4) * 10-5. Basing on our data and the known orbital period of the binary (Thorstensen and Fenton 2003) we calculate the period excess of 3.4 +/- 0.1%, which is typical for an SU UMa star at this orbital period. This value indicates that the mass ratio of the system is q=0.154.