The polarization of optical radiation from the magnetic white dwarfs

Details The polarization of optical radiation from the magnetic white dwarfs The polarization of optical radiation from the magnetic white dwarfs

Feb 1975

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1975ap%26ss..32..355s&link_type=abstract

Astrophysics and Space Science, vol. 32, Feb. 1975, p. 355-369.

Astronomy and Astrophysics

Astrophysics

13

Astronomical Models, Magnetic Stars, Optical Polarization, Stellar Radiation, White Dwarf Stars, Circular Polarization, Coronas, Cyclotron Radiation, Faraday Effect, Hot Electrons, Photosphere, Polarization Characteristics, Polarized Radiation, Scattering, Thermal Radiation

Scientific paper

It is pointed out that, because of the large Faraday rotation an outlet of linear polarization from the photosphere of a white dwarf is hampered. In accordance with this fact it is proposed to distinguish two types of magnetic white dwarfs. The first type (its representative is Grw 70°8247) has a linear polarization which is comparable in magnitude with the circular one. Polarization of radiation from the white dwarfs of the first type cannot arise in the photosphere. It arises in the corona of the star either as a result of cyclotron emission of hot electrons (T'%' 106 K) or as a result of scattering of slightly polarized emission from the photosphere in the corona. For the first type dwarfs such magnetic fields are required that 0B= wopt, i.e. B=(1-3) x 108 G. The white dwarfs of the second type (its representative is G 99-37) have their linear polarization much smaller than the circular one. Polariza- tion of these white dwarfs can arise as a result of the transfer of radiation in the nonisothermal photo- sphere. Magnetic fields required for the second type can be much smaller: B cos y=(l-lO) x 106 G. It is shown that the photospheric model allows to obtain the quantitative accordance of the theory with all the observational data for G 99-37 and is not in accordance with the data for Grw 7008247, at the same time the model with cyclotron emission from the corona explains the magnitude of both linear and circular polarization and their wavelength dependence for Grw 70°8247

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