A Dynamical Study of the Eclipsing Nova OY Arae

Details A Dynamical Study of the Eclipsing Nova OY Arae A Dynamical Study of the Eclipsing Nova OY Arae

Jul 1997

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997apj...483..899z&link_type=abstract

Astrophysical Journal v.483, p.899

Astronomy and Astrophysics

Astronomy

2

Stars: Binaries: Eclipsing, Stars: Individual Constellation Name: Oy Arae, Stars: Novae, Cataclysmic Variables, Stars: White Dwarfs

Scientific paper

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 H alpha 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&sun; and M2 ~ 0.34 M&sun;, 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.

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