Nitrogen recombination lines and abundance in nova shells

The observed intensities of N II lines in the DQ Her, CP Pup, and T Aur nova shells are compared with theoretical predictions. It is concluded that the relative intensities can be explained with excitation by recombination. The nitrogen abundances obtained from the line intensities relative to hydro...

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Bibliographic Details
Published inThe Astrophysical journal Vol. 369; no. 1; pp. 213 - 218
Main Authors ESCALANTE, V, DALGARNO, A
Format Journal Article
LanguageEnglish
Published Chicago, IL University of Chicago Press 01.03.1991
Subjects
640102 - Astrophysics & Cosmology- Stars & Quasi-Stellar, Radio & X-Ray Sources
ABUNDANCE
Astronomy
CHEMICAL COMPOSITION
CLASSICAL AND QUANTUM MECHANICS, GENERAL PHYSICS
COMPARATIVE EVALUATIONS
Earth, ocean, space
ELEMENT ABUNDANCE
ELEMENTS
ENERGY-LEVEL TRANSITIONS
ERUPTIVE VARIABLE STARS
Exact sciences and technology
EXCITATION
HYDROGEN
NITROGEN
NONMETALS
NOVAE
Novae, dwarf novae, recurrent novae, and other cataclysmic (eruptive) variables
NUCLEOSYNTHESIS
RECOMBINATION
STARS
SYNTHESIS
Variable and peculiar stars (including novae)
VARIABLE STARS
Atomic process
Intensity
Stellar abundance
Nova
Abundance ratio
Recombination line
Emission line
Nitrogen Positive ion
Circumstellar shell
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Summary:The observed intensities of N II lines in the DQ Her, CP Pup, and T Aur nova shells are compared with theoretical predictions. It is concluded that the relative intensities can be explained with excitation by recombination. The nitrogen abundances obtained from the line intensities relative to hydrogen have values about 400 to 700 times the solar abundance. 27 refs.
ISSN:0004-637X
1538-4357
DOI:10.1086/169752