Models of classical and recurrent novae

Details Models of classical and recurrent novae Models of classical and recurrent novae

Sep 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993nassp.507..371f&link_type=abstract

In NASA, Washington, Cataclysmic Variables and Related Objects p 371-412 (SEE N95-27068 09-89)

Computer Science

Light Curve, Novae, Stellar Envelopes, Stellar Mass Ejection, Stellar Models, Stellar Radiation, Stellar Spectra, Thin Walled Shells, Cataclysmic Variables, Electron Scattering, Optical Activity, Stellar Mass, Thickness

Scientific paper

The behavior of novae may be divided roughly into two separate stages: quiescence and outburst. However, at closer inspection, both stages cannot be separated. It should be attempted to explain features in both stages with a similar model. Various simple models to explain the observed light and spectral observations during post optical maximum activity are conceivable. In instantaneous ejection models, all or nearly all material is ejected in a time that is short compared with the duration of post optical maximum activity. Instantaneous ejection type 1 models are those where the ejected material is in a fairly thin shell, the thickness of which remains small. In the instantaneous ejection type 2 model ('Hubble Flow'), a thick envelope is ejected instantaneously. This envelope remains thick as different parts have different velocities. Continued ejection models emphasize the importance of winds from the nova after optical maximum. Ejection is supposed to occur from one of the components of the central binary, and one can imagine a general swelling of one of the components, so that something resembling a normal, almost stationary, stellar photosphere is observed after optical maximum. The observed characteristics of recurrent novae in general are rather different from those of classical novae, thus, models for these stars need not be the same.

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