The Accretion Disk in DQ HER
Abstract
The classical nova, DQ Her, shows rapid oscillations with a 71-sec period. These are low amplitude sinusoidal variations which (in this system) remain coherent for many years. In the present paper the intrinsic properties of DQ Her are examined. The oscillating part of the reflected light seen by an observer at an inclination angle is numerically computed, and the amplitude and phase of its fundamental and second harmonic is determined as a function of orbital phase of the binary system.
- Publication:
-
IAU Colloq. 53: White Dwarfs and Variable Degenerate Stars
- Pub Date:
- 1979
- Bibcode:
- 1979wdvd.coll..412P
- Keywords:
-
- Eclipsing Binary Stars;
- Novae;
- Stellar Mass Accretion;
- Stellar Oscillations;
- Stellar Rotation;
- White Dwarf Stars;
- Harmonics;
- Light Curve;
- Phase Shift;
- Stellar Radiation;
- Astrophysics