Classical novae and recurrent novae: General properties

Details Classical novae and recurrent novae: General properties Classical novae and recurrent novae: General properties

Sep 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993nassp.507..261h&link_type=abstract

In NASA, Washington, Cataclysmic Variables and Related Objects p 261-369 (SEE N95-27068 09-89)

Astronomy and Astrophysics

Astronomy

1

Astronomical Polarimetry, Cataclysmic Variables, Classifications, Novae, Spectrophotometry, Stellar Luminosity, Stellar Magnitude, Stellar Spectra, Visual Observation, Correlation, Dwarf Novae, Exosat Satellite, Heao 2, Imaging Techniques, Infrared Astronomy, Light Curve, Ultraviolet Astronomy, X Ray Astronomy

Scientific paper

We describe the observable characteristics of classical novae and recurrent novae obtained by different techniques (photometry, spectroscopy, and imaging) in all the available spectral ranges. We consider the three stages in the life of a nova: quiescence (pre- and post-outburst), outburst, final decline and nebular phase. We describe the photometric properties during the quiescent phase. We describe the photometric properties during outburst, the classification according the rate of decline (magnitudes per day), which permits us to define very fast, fast, intermediate, slow, and very slow novae and the correlation between luminosity and speed class. We report the scanty data on the spectra of the few known prenovae and those on the spectra of old novae and those of dwarf novae and nova-like, which, however, are almost undistinguishable. We describe the typical spectra appearing from the beginning of the outburst, just before maximum, up to the nebular phase and the correlation between spectral type at maximum, expansional velocity, and speed class of the nova. We report the existing infrared observations, which permit us to explain some of the characteristics of the outburst light curve, and give evidence of the formation of a dust shell in slow and intermediate novae (with the important exception of the very slow nova HR Del 1967) and its absence or quasi-absence in fast novae. The ultraviolet and X-ray observations are described. The X ray observations of novae, mainly from the two satellites EINSTEIN and EXOSAT, are reported. Observations of the final decline and of the envelopes appearing several months after outburst are also reported.

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