http://arxiv.org/abs/1507.03070
We derive the transfer equations for polarized radiation in the atmospheres of compact stars, which take into account a frequency redistribution of radiation within and near a cyclotron line core. The equations are valid in the magnetic fields up to $10^{13}$ G and can be used for numerical modeling of a cyclotron line formation in the warm magnetospheric plasmas of compact stars.
We present two forms of such equations. The first form, for the intensities of ordinary and extraordinary modes, is applicable for the compact stars with a moderate magnetic field strength up to $10^{10}-10^{11}$ G. The second form, for the Stokes parameters, is more complex, but applicable even if a linear mode coupling takes place somewhere in the scattering-dominated atmosphere. Analysing dispersion properties of a magnetized plasma, we show that the linear mode coupling is possible for a wide range of parameters and originates from a partial cancellation of the plasma and vacuum contributions to the refraction indices.
M. Garasev, E. Derishev, V. Kocharovsky, et. al.
Tue, 14 Jul 15
49/64
Comments: 10 pages, 1 figure
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