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Influence of the Magnetic Field on the Polarization of Radiation Scattered by Electrons in Stellar Atmospheres and Envelopes

Published online by Cambridge University Press:  12 April 2016

A.Z. Dolginov ,
Yu.N. Gnedin  and
N.A. Silant’ev
A.Z. Dolginov
Affiliation:
A. F. Ioffe Institute of Physics and Technology, 194021 Leningrad, USSR
Yu.N. Gnedin
Affiliation:
Central Astronomical Observatory at Pulkovo, 196140 Leningrad, USSR
N.A. Silant’ev
Affiliation:
Central Astronomical Observatory at Pulkovo, 196140 Leningrad, USSR

Extract

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The radiation scattering by electrons play an important role for stars with the surface temperature ≥ 2.104 °K. Many among these stars have magnetic fields of the order 1 - 100 G. We shall consider the role of the field for the radiative transfer in continuum spectra.

Electrons in the field form an axisymmetric medium similar to the single axis crystal. Hence, the medium will have dichroism and birefringency. If the gyrofrequency ωB is much less than the radiation frequency ω then the dichroism can be neglected. The circular birefringency can be characterized by the angle of the Faraday rotation

Type
Section I - Theoretical Considerations
Information
International Astronomical Union Colloquium , Volume 90: Upper Main Sequence Stars with Anomalous Abundances , 1986 , pp. 81 - 86
Copyright
Copyright © Reidel 1986

References

Chandrasekhar, S., 1950, Radiative Transfer, Oxford.Google Scholar
Dolginov, A.Z., and Silant’ev, N.A., 1979, Pisma v Astron. Journal (in Russian), 5, 526.Google Scholar
Gnedin, Yu.N., and Silant’ev, N.A., 1980, Pisma v Astron. Journal (in Russian), 6, 344.Google Scholar
Gnedin, Yu.N., and Silant’ev, N.A., 1984, Astrophys. Space Sci., 102, 375.Google Scholar
Sobolev, V.V., 1956, Radiative Transfer in the Atmospheres of Stars and Planets (in Russian), Moscow.Google Scholar