Spherically symmetric, expanding, non-LTE model atmospheres for novae during their early stages

Details Spherically symmetric, expanding, non-LTE model atmospheres for novae during their early stages Spherically symmetric, expanding, non-LTE model atmospheres for novae during their early stages

Jul 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992apj...393..307h&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 393, no. 1, July 1, 1992, p. 307-328. Research supported by Institute of Ge

Physics

Geophysics

51

Cataclysmic Variables, Nonequilibrium Thermodynamics, Photosphere, Stellar Atmospheres, Stellar Models, Abundance, Balmer Series, Iue, Novae, Stellar Spectrophotometry

Scientific paper

In the continuum and line-blanketed models presented here, nova atmospheres are characterized by a very slow decrease of density with increasing radius. This feature leads to very large geometrical extensions so that there are large temperature differences between the inner and outer parts of the line-forming regions. The theoretical spectra show a large IR excess and a small Balmer jump which may be either in absorption or in emission. For the parameters considered (effective temperature of about 10 exp 4 K, L = 2 x 10 exp 4 solar luminosities, outer boundary density of about 3 x 10 exp -15 g cm exp -3, mass-loss rate of 10 exp -5 solar masses/yr), most lines are in absorption. The effects of changes in the abundances of the heavy elements on the emergent spectra are discussed. The strong unidentified features observed in ultraviolet spectra of novae are found in actuality to be regions of transparency within the Fe 'forest'. Ultraviolet spectra obtained from the IUE archives are displayed, and spectral synthesis of these spectra is done using the theoretical atmospheres.

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