The chemical composition of the emitting gas in HM Sagittae

Details The chemical composition of the emitting gas in HM Sagittae The chemical composition of the emitting gas in HM Sagittae

Feb 1989

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1989apj...337..520d&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 337, Feb. 1, 1989, p. 520-527.

Astronomy and Astrophysics

Astrophysics

10

Astronomical Spectroscopy, Binary Stars, Emission Spectra, Stellar Composition, Symbiotic Stars, Abundance, Chemical Composition, Electron Density (Concentration), M Stars, Mira Variables, Red Giant Stars, White Dwarf Stars

Scientific paper

Spectroscopic observations of HM Sge obtained in 1985 and 1986 using a 1.6-m telescope with a 0.5-A resolution are reported. It is found that the broad line component is formed in a region characterized by an electron temperature of 14,000 to 15,000 K and an electron density of 33,700,000/cu cm. Helium overabundance and nitrogen enhancement are observed in the emitting gas. It is shown that the source has a temperature of about 180,000 K and a radius and luminosity comparable to those of the central stars of planetary nebulae.

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