A Dynamical Study of the Eclipsing Nova OY Arae
Abstract
Photometric and spectroscopic observations of the classical nova OY Ara were carried out using the Cerro Tololo Inter-American Observatory telescopes. We found that OY Ara is an eclipsing system with an orbital period of 0.155466 +/- 0.000003 days. The radial velocity semiamplitude of the Hα emission line is 118 +/- 9 km s-1. Assuming the secondary is near the main sequence, the dynamical analysis shows that the primary and the secondary have masses of M1 ~ 0.82 M⊙ and M2 ~ 0.34 M⊙, respectively. We also find that the accretion disk of OY Ara is 2.5-6 mag more luminous than that of the X-ray novae, presumably due to the much higher rate of mass transfer in classical novae.
- Publication:
-
The Astrophysical Journal
- Pub Date:
- July 1997
- DOI:
- 10.1086/304283
- Bibcode:
- 1997ApJ...483..899Z
- Keywords:
-
- Stars: Binaries: Eclipsing;
- Stars: Novae;
- Cataclysmic Variables;
- stars: individual (OY Ara);
- Stars: White Dwarfs