Large-Amplitude 2.65-d Oscillation in the VY Scl-Type star V425 Cas
Abstract
From long-term photometry of a VY Scl-type star, V425 Cas, between 1998 and 2000, we discovered a short-term, large-amplitude (up to 1.5 mag) variations. The variation was well represented by a single period of 2.65 d. The large amplitude and the profile of the folded light curve suggest that the dwarf nova-type disk instability is responsible for this variation. The shortness of the period is unprecedented in hydrogen-rich cataclysmic variables. Given the recent emerging evidence that the irradiation from white dwarfs in VY Scl-type systems affect their light behavior, we propose a possibility that this unique variation in V425 Cas can be explained by the combination of the dwarf nova-type disk instability and irradiation. Similar short-period "outbursts" have been known in X-ray transients (V518 Per), and helium cataclysmic variables (CR Boo and V803 Cen). We discuss the possibility that these phenomena have a common origin to the unique variation in V425 Cas.
Keywords
Cite
@article{arxiv.astro-ph/0110240,
title = {Large-Amplitude 2.65-d Oscillation in the VY Scl-Type star V425 Cas},
author = {Taichi Kato and Makoto Uemura and Ryoko Ishioka and Timo Kinnunen},
journal= {arXiv preprint arXiv:astro-ph/0110240},
year = {2015}
}
Comments
6 pages, 5 figures, accepted for publication in Publ. Astron. Soc. Japan