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Title:
The neon nova. II - Condensation of silicate grains in the ejecta of Nova Vulpeculae 1984 number 2
Authors:
Gehrz, R. D.; Grasdalen, G. L.; Greenhouse, M.; Hackwell, J. A.; Hayward, T.; Bentley, A. F.
Affiliation:
AA(Minnesota, University, Minneapolis), AB(Wyoming Infrared Observatory, Laramie), AC(Wyoming Infrared Observatory, Laramie), AD(Wyoming Infrared Observatory, Laramie), AE(Aerospace Corp., Space Sciences Laboratory, Los Angeles, CA)
Publication:
Astrophysical Journal, Part 2 - Letters to the Editor (ISSN 0004-637X), vol. 308, Sept. 15, 1986, p. L63-L66. Research supported by the University of Minnesota. (ApJL Homepage)
Publication Date:
09/1986
Category:
Astrophysics
Origin:
STI
NASA/STI Keywords:
COSMOCHEMISTRY, INFRARED SPECTRA, NOVAE, SILICATES, STELLAR MASS EJECTION, STELLAR SPECTROPHOTOMETRY, ABUNDANCE, BINARY STARS, SPECTRAL RESOLUTION, STELLAR COMPOSITION, STELLAR EVOLUTION, WHITE DWARF STARS
DOI:
10.1086/184745
Bibliographic Code:
1986ApJ...308L..63G

Abstract

Infrared photometry of Nova Vulpeculae 1984 number 2 (NV2) from 2.3 to 19.5 microns during May 14, 1985 to March 31, 1986 shows that silicate grains had condensed and grown in the nova ejecta by August 23, 1985, 240 days after the eruption. A relative overabundance of oxygen in the nova shell seems indicated. Forbidden 12.8-micron Ne II forbidden line emission was a factor of about 41 above the continuum at a spectral resolution of 67 on day 240; the line persisted through day 461. The anomalous chemical composition of NV2's ejecta supports recent suggestions that ONeMg white dwarfs (evolved from 8-12 solar-mass progenitor stars) are accreting matter in binary systems.

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