The masses of V838 Herculis (Nova Herculis 1991) and OZ Aurigae

Details The masses of V838 Herculis (Nova Herculis 1991) and OZ Aurigae The masses of V838 Herculis (Nova Herculis 1991) and OZ Aurigae

Jan 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994apj...420..830s&link_type=abstract

The Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 420, no. 2, p. 830-836

Astronomy and Astrophysics

Astrophysics

13

Eclipsing Binary Stars, Radial Velocity, Stellar Mass, White Dwarf Stars, Accretion Disks, H Alpha Line, Stellar Models, Stellar Structure

Scientific paper

We have determined H alpha radial velocity solutions for the two eclipsing novae V838 Her (Nova Her 1991) and QZ Aur, which yields mass estimates for the stellar components. The results indicate both objects have relatively massive white dwarfs greater than 0.62 solar mass for V838 Her and greater than 0.65 solar mass for QZ Aur), although these limits allow lower masses than theoretical models for fast novae predict. Even though both novae have long periods (7.14 hr and 8.58 hr), there is no visible evidence of the secondary star in the spectrum. The large extent and brightness of the accretion disk, as deduced from the light curves, make the disk the dominant source of light.

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