Infrared emission by dust grains near variable primary sources. II - A model for infrared novae

Details Infrared emission by dust grains near variable primary sources. II - A model for infrared novae Infrared emission by dust grains near variable primary sources. II - A model for infrared novae

Sep 1980

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1980a%26a....89..158b&link_type=abstract

Astronomy and Astrophysics, vol. 89, no. 1-2, Sept. 1980, p. 158-168.

Astronomy and Astrophysics

Astronomy

21

Cosmic Dust, Emission Spectra, Infrared Astronomy, Novae, Stellar Envelopes, Stellar Spectrophotometry, Light Curve, Radiant Flux Density, Stellar Luminosity, Stellar Models, Ultraviolet Absorption

Scientific paper

The observational data on the visual, infrared and ultraviolet behavior of the Novae Serpentis 1970 and Aquilae 1975 after outburst are reviewed. In common with several other workers, it is suggested that the grains giving rise to the well-known infrared development of novae already exist near nova progenitors prior to outburst, and that the evidence for the rapid formation of grains after outburst is not convincing. It is proposed that these pre-existing grains are small (0.01 micron) and that their ultraviolet absorbing efficiency, combined with the constant bolometric luminosity nova model of Bath and Shaviv (1976) provides a natural explanation for the infrared behavior of novae. The model, together with the principles outlined in the first paper of this series, enables the production of detailed infrared light curves, at all relevant wavelengths, that closely match the infrared development of Novae Serpentis and Aquilae. Some possible methods of verifying the model observationally are suggested.

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