During the outburst of V713 Cephei in August 2009 the times of 8 eclipses were measured and these, together with 5 eclipse timings obtained during quiescence in August 2007, provide an improved orbital period of 0.085418432(4)d. No superhumps were observed in the light curve indicating this was a normal UG-type dwarf nova outburst. We found the eclipse depth decreased linearly with rising system excitation level, falling from ~3 magnitudes in quiescence to ~2 magnitudes during outburst. The depth and totality of eclipses in quiescence suggests a high orbital inclination. We saw no variation in the FWHM of eclipses between quiescence and outburst despite a significant change in shape of the eclipse profile.
@article{arxiv.1012.0138,
title = {The outburst of V713 Cephei in August 2009},
author = {David Boyd and Denis Denisenko and Robert Koff and Ian Miller and Bart Staels},
journal= {arXiv preprint arXiv:1012.0138},
year = {2011}
}
Comments
9 pages, 9 figures, accepted for publication in the Journal of the British Astronomical Association