The Orbital Period and Negative Superhumps of the Nova-Like Cataclysmic Variable V378 Pegasi

Abstract

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.

24 pages, 19 figures, accepted for publication in New Astronomy

References in corpus (2)

• Spatial distribution and galactic model parameters of cataclysmic variables
• A new absolute magnitude calibration with 2MASS for cataclysmic variables

Cited by in corpus (5)

• TESS light curves of cataclysmic variables -- II: Superhumps in old novae and novalike variables
• Discovery of Negative Superhumps during a Superoutburst of January 2011 in ER Ursae Majoris
• Study of Negative and Positive Superhumps in ER Ursae Majoris
• Exploring the tilted accretion disc of AQ Men with TESS
• Tilt, Warp, and Simultaneous Precessions in Disks