Ultraviolet spectral evolution and heavy element abundances in Nova Austrinae 1981

Details Ultraviolet spectral evolution and heavy element abundances in Nova Austrinae 1981 Ultraviolet spectral evolution and heavy element abundances in Nova Austrinae 1981

Feb 1985

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985mnras.212..753w&link_type=abstract

Monthly Notices of the Royal Astronomical Society (ISSN 0035-8711), vol. 212, Feb. 15, 1985, p. 753-766. Research supported by t

Astronomy and Astrophysics

Astronomy

81

Heavy Elements, Stellar Composition, Stellar Evolution, Stellar Spectra, Ultraviolet Astronomy, Gas Ionization, Spectrum Analysis, White Dwarf Stars

Scientific paper

Nova CrA 1981, a moderately fast galactic nova, was systematically observed over a period of seven months with the IUE satellite. The initial evolution of the UV spectrum was similar to that of previously observed novae; however, several months after maximum, weak emission due to very high ionizating forbidden lines of Na, Mg, Al, and Si appeared, eventually decreasing in strength over the next two months. The spectral development of the lines is consistent with the photoionization of an expanding shell; a high-temperature 'coronal' origin is ruled out. Abundances deduced from the spectra show that most of the observed heavy elements in the ejected material are enhanced with respect to helium, with neon the most abundant of these. In addition, there are substantial deviations of the Na/Mg/Al/Si abundance ratios from solar values. This is interpreted as evidence for the mixing of core material with the accreted envelope on a massive O-Ne-Mg (as opposed to a C-O) white dwarf. Furthermore, the proportion of core material in the ejecta implies that the mass of the white dwarf decreased as a consequence of the outburst.

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