Polarization of intrinsic radiation of tidally distorted stars with electron-scattering atmospheres. II - an account of true absorption

Details Polarization of intrinsic radiation of tidally distorted stars with electron-scattering atmospheres. II - an account of true absorption Polarization of intrinsic radiation of tidally distorted stars with electron-scattering atmospheres. II - an account of true absorption

Feb 1985

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985ap%26ss.109....1b&link_type=abstract

Astrophysics and Space Science (ISSN 0004-640X), vol. 109, no. 1, Feb. 1985, p. 1-14.

Astronomy and Astrophysics

Astrophysics

3

Atmospheric Scattering, Atmospheric Tides, Electron Scattering, Linear Polarization, Stellar Atmospheres, Stellar Radiation, Albedo, Atmospheric Models, Binary Stars, Limb Darkening, Roche Limit

Scientific paper

Linear polarization of radiation emitted by tidally distorted stars as a function of the binary system phase is computed, taking into account true absorption and the scattering of light on free and bound electrons within hot stellar atmospheres. Computations are made both for the linear distribution of true sources across the atmospheres and for radiative-stable model atmospheres presented by Kurcuz et al. (1974) and Kurucz (1979). Polarization variability was investigated as a function of wavelength t. In a number of cases, polarization variability was found to be at an observable level. The most marked variability was expected in the ultraviolet range adjacent to the boundaries of the spectral series for H and He. Near the Lyman limit of approximately ~ = 912 A for stars with an effective temperature TCff ~ 35000 K and near the ionization boundary for He ii 226 A for stars with Teff> 35000 K, the amplitude of polarization variability is greater than in the case of pure electron atmospheres, sometimes reaching the level of 0.5-1 0/~* For fairly long waves where the limb-darkening coefficient falls below a certain critical value Ucr 0.5, the plane of polarization is found to be turned by 900 as compared to the case of a pure electron atmosphere. For limb-darkening coefficients far from the value of ucr; the form of the polarization phase curves, as well as dependence on the parameters of a binary system, remain approximately the same as those in the case of pure electron scattering

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