Temperature and luminosity of hot components in symbiotic stars

Details Temperature and luminosity of hot components in symbiotic stars Temperature and luminosity of hot components in symbiotic stars

Aug 1991

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991a%26a...248..458m&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 248, no. 2, Aug. 1991, p. 458-474. Research supported by SNSF.

Astronomy and Astrophysics

Astrophysics

183

Hot Stars, Stellar Luminosity, Stellar Temperature, Symbiotic Stars, Hertzsprung-Russell Diagram, Iue, Planetary Nebulae, Red Giant Stars, Stellar Mass Ejection, Stellar Spectra, White Dwarf Stars

Scientific paper

Typical radiation temperatures and luminosities are derived for the hot component of a representative sample of symbiotic systems by adapting the Zanstra method to the special requirements of symbiotic stars. Temperatures are derived by comparing the He II 1640 nebular recombination line with the underlying continuum. Particle-bounded and radiation-bounded nebulae are differentiated by comparing the continuum flux at 1640 A with the nebular Balmer continuum at the long end of the IUE wavelength range. Interstellar extinctions are determined as well. Mass-loss rates for the red giants are determined where the binary periods are known. It is inferred that the hot components in symbiotic systems lie on the post-red-giant track. In some cases this may be a white dwarf; in others it may be closer to the central star of a planetary nebula, and in still others it is a white dwarf in a slow nova-like outburst, which may last for decades.

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