Rapid spectral variations of old novae.

Details Rapid spectral variations of old novae. Rapid spectral variations of old novae.

Jun 1988

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1988msngr..52...49f&link_type=abstract

The Messenger, vol. 52, p. 49-50

Computer Science

2

Nova Puppis 1942, Novae:Spectral Variations

Scientific paper

Novae are a subclass of cataclysmic variables. The latter all appear to be binary with a white dwarf component and a companion usually near the main sequence. This companion seems to fill its Roche lobe and lose mass to the white dwarf via the inner Lagrangian point. Unless the magnetic field of the white dwarf is very strong, the transferred mass is expected to spiral slowly to the white dwarf in an accretion disk, whose presence explains many observations. Different kinds of cataclysmic variable exist, such as different sorts of dwarf novae with outbursts generally having an amplitude of a few magnitudes at intervals of the order of weeks. The orbital periods determined up to April 1987 (Ritter 1987) lie between 2.00 days (the nova GK Per) and 0.052 days (the dwarf nova AF Cam), with a "period gap" between 0.118 and 0.086 days (only one known period inside the gap).

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