The optical spectrum of FG Sagittae during its recent decline in brightness

Details The optical spectrum of FG Sagittae during its recent decline in brightness The optical spectrum of FG Sagittae during its recent decline in brightness

Jul 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993pasp..105..755s&link_type=abstract

Astronomical Society of the Pacific, Publications (ISSN 0004-6280), vol. 105, no. 689, p. 755-760.

Astronomy and Astrophysics

Astronomy

22

Peculiar Stars, Planetary Nebulae, Stellar Luminosity, Variable Stars, Visible Spectrum, Absorption Spectra, Stellar Color, Stellar Models, Stellar Spectra, Stellar Spectrophotometry

Scientific paper

We describe low- and intermediate-resolution optical spectra of the peculiar variable star FG Sagittae that were obtained during the later stages of its current episode of sharply diminished optical luminosity. In the region from 5600 to 6700 A, the line spectrum is essentially the same as it was in 1983: it contains lines of Fe-peak elements typical of luminous stars of spectral type G or early K, together with a forest of lines due to heavy elements associated with traditional s-process species, e.g., Zr, Ba, Ce, La, Sm, and Y. Estimates of (B - V), derived from these flux-calibrated spectra, show that from early November 1992 onward, the continuum grew progressively redder until by the end of 1992, the color of the central star became even redder than it was before the onset of the current episode. The present results are compatible with a model in which the diminution in optical luminosity is the result of the ejection of a semitransparent dust shell by the central star, as proposed by Woodward et al. (1993). There is no compelling evidence to suggest that the central star is returning to its pre-1960 state within the domain of hot stars.

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