F. A. Ringwald, Kenia Velasco, Jonathan J. Roveto, Michelle E. Meyers
A radial velocity study is presented of the cataclysmic variable V378 Pegasi
(PG 2337+300). It is found to have an orbital period of 0.13858 +/- 0.00004 d
(3.32592 +/- 0.00096 hours). Its spectrum and long-term light curve suggest
that V378 Peg is a nova-like variable, with no outbursts. We use the
approximate distance and position in the Galaxy of V378 Peg to estimate E(B-V)
= 0.095, and use near-infrared magnitudes to calculate a distance of 680 +/- 90
pc and M_V = 4.68 +/- 0.70, consistent with V378 Peg being a nova-like.
Time-resolved photometry taken between 2001 and 2009 reveals a period of 0.1346
+/- 0.0004 d (3.23 +/- 0.01 hours). We identify this photometric variability to
be negative superhumps, from a precessing, tilted accretion disk. Our repeated
measurements of the photometric period of V378 Peg are consistent with this
period having been stable between 2001 and 2009, with its negative superhumps
showing coherence over as many as hundreds or even thousands of cycles.
View original:
http://arxiv.org/abs/1111.3677
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