HM Sagittae - Symbiotic cousin of the RS CVn stars

Details HM Sagittae - Symbiotic cousin of the RS CVn stars HM Sagittae - Symbiotic cousin of the RS CVn stars

Jun 1981

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1981a%26a....99...73b&link_type=abstract

Astronomy and Astrophysics, vol. 99, no. 1, June 1981, p. 73-79.

Astronomy and Astrophysics

Astrophysics

24

Binary Stars, Planetary Nebulae, Stellar Envelopes, Stellar Evolution, Stellar Mass Ejection, Stellar Spectrophotometry, Abundance, Density Distribution, Giant Stars, Helium, Interstellar Extinction, Line Spectra, Stellar Oscillations, Temperature Distribution, Visible Spectrum

Scientific paper

In the brief time since its brightening in 1975, the optical spectrum of HM Sagittae has shown considerable variation in both its general characteristics and relative line intensity ratios. The observations place HM Sagittae in a small class of objects which are thought to be proto-planetary nebulae, of which V 1016 Cygni is the prototype. Attention is given to derived density and temperature, helium abundance and nebular mass, and an evolutionary scenario. The considered observations show a decrease in the intensity of the continuum and a continuation of the trend toward higher excitation in the spectrum of HM Sagittae. Parallels are seen in the development of this object and V 1016 Cygni, with the implication that the trend toward higher excitation is expected to continue.

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