The abundances of the elements -carbon to silicon- in Nova Corona Austrina 1981

Details The abundances of the elements -carbon to silicon- in Nova Corona Austrina 1981 The abundances of the elements -carbon to silicon- in Nova Corona Austrina 1981

Dec 1984

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984nascp2349..309s&link_type=abstract

In NASA. Goddard Space Flight Center Future of Ultraviolet Astronomy Based on Six Years of IUE Res. p 309-312 (SEE N85-20961 1

Astronomy and Astrophysics

Astronomy

Carbon, Novae, Silicon, Binary Stars, Forbidden Bands, Iue, Stellar Evolution, Stellar Spectra, White Dwarf Stars

Scientific paper

Nova Corona Austrina 1981 was observed systematically over a period of seven months with the IUE satellite. These spectra cover the range 1150-3200 A, and are mostly at low dispersion. The emission lines identified in the low dispersion spectra cover a range in ionization potential from about 8 ev (Mg II) to about 80 ev (N V). Line emission fluxes and widths were measured in all spectra. Several months after maximum visual light, high ionization forbidden lines of sodium, magnesium, and aluminum appeared and then declined over a period of two months. The abundances deduced from these lines imply that nitrogen, oxygen, neon, sodium, magnesium, and aluminum are all enhanced with respect to helium while carbon is not. The observations of this nova, plus the observations of Nova Cygni 1975 and Nova Aquila 1982, imply that some fraction of novae contain white dwarfs that underwent non-degenerate carbon burning prior to entering a close binary-nova phase of evolution.

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