The Spectrum of the Symbiotic Nova AS 296 (=FG Serpentis) from 1988 July to 1992 March

Within about a month after its 1988 outburst, AS 296 showed a strong continuum, emission lines of singly ionized metals, and deep absorption lines also of the ionized metals. The emission lines indicate an expansion velocity of only about 50 km s⁻ⁱ. The absorption lines are those of high-density she...

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Bibliographic Details
Published in:Publications of the Astronomical Society of the Pacific 1993-08, Vol.105 (690), p.859-862
Main Authors: Wallerstein, George, Gilroy, Kalpana Krishaswamy, Willson, L. A., Garnavich, Peter
Format: Article
Language:English
Subjects:
Astronomy
Binary and multiple stars
Cataclysmic binaries (novae, dwarf novae, recurrent novae, and nova-like objects). Symbiotic stars
Continuous spectra
Diffuse interstellar bands
Earth, ocean, space
Emission spectra
Exact sciences and technology
Line spectra
Novae
Novae, dwarf novae, recurrent novae, and other cataclysmic (eruptive) variables
Radial velocity
Stars
Stellar spectra
Symbiotic stars
Variable and peculiar stars (including novae)
Wavelengths
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Summary:Within about a month after its 1988 outburst, AS 296 showed a strong continuum, emission lines of singly ionized metals, and deep absorption lines also of the ionized metals. The emission lines indicate an expansion velocity of only about 50 km s⁻ⁱ. The absorption lines are those of high-density shell as indicated by the presence of Mg 4481 A, and the absence of Sr 4215 A. In 1991 and 1992, low-to-medium excitation forbidden emission lines had appeared. An analysis of the diffuse interstellar bands in absorption indicates a reddening of 0.35 ± 0.05 mag, which is considerably less than assumed by Munari et al. (1992).
ISSN:0004-6280
1538-3873
DOI:10.1086/133245