Physics
Scientific paper
Apr 1987
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987azh....64..373t&link_type=abstract
Astronomicheskii Zhurnal (ISSN 0004-6299), vol. 64, Mar.-Apr. 1987, p. 373-392. In Russian.
Physics
3
Carbon Stars, Electrophotometry, Lunar Occultation, Stellar Occultation, Stellar Physics, Diameters, Diffraction Patterns, Spectral Bands, Spectral Energy Distribution
Scientific paper
From the analysis of the diffraction pattern registered in the R spectral band (λ0 ≅ 7000 Å) during the observation of the lunar occultation of the carbon star Y Tau the angular diameter of the star is determined: d = 0arcsec.0056±0arcsec.0012. The value obtained is approximately 1.5 times less than the angular diameter measured in the near-infrared range (λ0 = 1.64 μm) during the observations of the occultations of Y Tau by the Ridgway group. The value of the angular diameter presented above corresponds to the star's photosphere, and the value ds = 0arcsec.00858±0arcsec.00040 determined by Ridgway et al., is related to the layer of the dust shell or the level of the extended atmosphere, which radiates most intensely in the near-infrared range. The temperature at the photosphere level is apparently close to Tp ≅ 2700 - 2800K, the characteristic temperature of the radiation of the shell (or extended atmosphere) is Ts ≅ 2000 - 2300K and the effective temperature of the star corresponding to the angular diameter ds is Te = 2595±75K. The absolute bolometric magnitude of Y Tau is Mb ≅ -5m.2, the bolometric luminosity is Lb ≅ 3.6×1037erg/s, the photosphere radius is Rp ≅ (315±80) R_sun;, the radius of the emitting layer of the shell (or atmosphere) which was observed during the occultations is Rs ≅ (485±45) R_sun;.
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