Statistics – Computation
Scientific paper
Apr 1991
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991apjs...75.1293w&link_type=abstract
Astrophysical Journal Supplement Series (ISSN 0067-0049), vol. 75, April 1991, p. 1293-1322.
Statistics
Computation
21
Computational Astrophysics, Magnetic Stars, Radiative Transfer, Stellar Magnetic Fields, Thomson Scattering, White Dwarf Stars, Circular Polarization, Cyclotron Radiation, Field Strength, Linear Polarization, Monte Carlo Method, Stellar Atmospheres
Scientific paper
The Monte Carlo method is used here to solve the radiative transfer equation for Thomson scattering in a constant magnetic field perpendicular to the atmosphere. Emergent radiation and polarization are presented for various atmospheric thicknesses. The circular polarization peaks at frequencies near the cyclotron, omega(c), and for propagation direction along the field. At low field strengths, the circular polarization is roughly proportional to omega(c)/omega; the linear polarization is proportional to the square of omega(c)/omega and the amount of circular polarization present at each scatter and is therefore much smaller than the circular polarization. The linear polarization is large for propagation direction perpendicular to the magnetic field and at frequencies near the cyclotron and in the strong-field limit. The position angle of the linear polarization undergoes a rotation of 90 deg at a value of omega(c)/omega near the square root of three.
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