Astronomy and Astrophysics – Astrophysics
Scientific paper
Aug 1987
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987a%26a...182...51n&link_type=abstract
Astronomy and Astrophysics (ISSN 0004-6361), vol. 182, no. 1, Aug. 1987, p. 51-62. SNSF-supported research.
Astronomy and Astrophysics
Astrophysics
104
Stellar Activity, Stellar Mass Accretion, Symbiotic Stars, Photons, Stellar Evolution, Stellar Spectra, Stellar Winds
Scientific paper
Symbiotic stars are assumed to be double star systems. It is shown with detailed model calculations that a typical outbreak of a symbiotic star can be induced by an increase in the mass loss of the cool star. The onset of that stellar wind will provide a fast increasing target for the photons emitted by the hot star. The cool stellar wind is ionized by the radiation of the hot companion. Depending on the temperature of the hot star, the mass loss, and the stellar separation, the emission of the low- and medium-ionized atoms may originate at various regions between the cool and the hot star. Differences in the combination of mass loss, stellar separation, and radiation temperature may also explain the observationally established division of symbiotic stars into s-type and d-type. The evolution of M(B) and M(V) is calculated as a function of the mass loss of the cool star. The calculated line profiles show periodic variations in intensity and wavelength position, as seen in several symbiotic stars (e.g., HBV 475).
Nussbaumer Harry
Vogel Manfred
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