V795 Herculis (=PG 1711+336), A Peculiar Intermediate Polar without Strong X-Ray Emission
Abstract
Additional photometry of V795 is obtained to determine the coherence of the 2.8-hr modulation and establish whether it is truly periodic or only quasi-periodic. The ephemeris for the photometric period is revised. The period is highly stable; the upper limit to the rate of change of the period is less than 1.7 x 10 exp -9. Quasi-periodic oscillations with periods near 1000 s are found. It is argued on theoretical and observational grounds that accretion disks cannot have stable precession periods. As the clock that underlies the 2.8-hr photometric modulation is highly stable, it is concluded that the modulation is not caused by a precessing disk, that the intermediate polar model remains the most viable model for V795 Her, and that intermediate polars need not be strong X-ray sources.
- Publication:
-
The Astrophysical Journal
- Pub Date:
- November 1991
- DOI:
- 10.1086/170677
- Bibcode:
- 1991ApJ...381..534Z
- Keywords:
-
- Cataclysmic Variables;
- Dwarf Novae;
- Hercules Nova;
- Peculiar Stars;
- Exosat Satellite;
- X Rays;
- Astrophysics;
- STARS: DWARF NOVAE;
- STARS: INDIVIDUAL CONSTELLATION NAME: V795 HERCULIS