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Title:
The peculiar infrared temporal development of Nova Vulpeculae 1987 (QV Vulpeculae)
Authors:
Gehrz, R. D.; Jones, T. J.; Woodward, C. E.; Greenhouse, M. A.; Wagner, R. M.; Harrison, T. E.; Hayward, T. L.; Benson, J.
Affiliation:
AA(Minnesota Univ., Minneapolis), AB(Minnesota Univ., Minneapolis), AC(Wyoming Infrared Observatory, Laramie), AD(National Air and Space Museum, Washington), AE(Ohio State Univ., Columbus), AF(Mount Stromlo and Siding Spring Observatories, Canberra, Australia), AG(Cornell Univ., Ithaca, NY), AH(Wyoming Infrared Observatory, Laramie)
Publication:
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 400, no. 2, p. 671-680. (ApJ Homepage)
Publication Date:
12/1992
Category:
Astrophysics
Origin:
STI
NASA/STI Keywords:
ASTRONOMICAL SPECTROSCOPY, COSMIC DUST, INFRARED ASTRONOMY, NOVAE, PECULIAR STARS, ASTRONOMICAL PHOTOMETRY, CATACLYSMIC VARIABLES, STELLAR ENVELOPES, VISIBLE SPECTRUM
DOI:
10.1086/172029
Bibliographic Code:
1992ApJ...400..671G

Abstract

The paper reports 1.25-19.5-micron IR photometry and optical/IR spectroscopy of Nova QV Vul (1987) from November 1987 through September 1989. The measurements show that an optically thick carbon dust shell formed within 83 d of the outburst, and that the spectral signatures of four types of astrophysical grains appeared at various times during a 2-yr period following the eruption. Carbon, SiC, and hydrocarbons formed first; oxygen-rich silicates formed later. It is suggested that the carbon dust components formed in fast-moving polar flumes, and that the silicates formed in a slow-moving equatorial ring. Mass estimates from the IR photometry and optical spectroscopy confirm that grain condensation in both the slow and fast ejecta of QV Vul is consistent with constraints established by previous observations of other dusty novae. It is concluded that the condensible elements in these grains were present in approximately solar abundance.

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