Spectroscopic observations of the symbiotic binary RW Hydrae

Details Spectroscopic observations of the symbiotic binary RW Hydrae Spectroscopic observations of the symbiotic binary RW Hydrae

May 1987

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987apj...316..427k&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 316, May 1, 1987, p. 427-433. Research supported by the U.S.-Spanish Joint

Physics

16

Binary Stars, Spectral Energy Distribution, Stellar Physics, Stellar Spectra, Stellar Spectrophotometry, Symbiotic Stars, H Ii Regions, Infrared Photometry, Red Giant Stars, Stellar Temperature, Ultraviolet Spectroscopy, Visible Spectrum

Scientific paper

Ultraviolet/optical spectrophotometry and infrared photometry show that the symbiotic binary RW Hya is comprised of an M giant (with L of about 1000 solar luminosities) and a compact object (with L of about 200 solar luminosities) which resembles the central star of a planetary nebula. The luminosity of the hot component is produced by a nuclear shell source which is replenished by the wind of the red giant at a rate of about 10 to the -8th solar mass/yr. Results indicate that the binary is surrounded by an H II region (of radius of about 10 AU) which gives rise to the observed emission lines and radio emission. The He(2+) and O(2+) regions are found to be confined to the immediate vicinity of the hot component.

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