Transfer of Polarized Radiation - Practical Experience with the Accelerated Lambda Iteration Method

Details Transfer of Polarized Radiation - Practical Experience with the Accelerated Lambda Iteration Method Transfer of Polarized Radiation - Practical Experience with the Accelerated Lambda Iteration Method

Jan 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003aspc..288..617d&link_type=abstract

Stellar Atmosphere Modeling, ASP Conference Proceedings, Vol. 288. Abstracts from a conference held 8-12 April 2002 in Tuebingen

Astronomy and Astrophysics

Astronomy

1

Scientific paper

Neutron stars and some of the white dwarfs have magnetic fields. The light emitted by these stars is polarized and can be characterized by the four Stokes components I, Q, U, and V. Therefore the polarized radiation transport equation differs significantly from the non-magnetic case. It is a system of linear differential equations coupled in I, Q, U, and V with depth dependent opacities and magneto-optical parameters. The most potential method, the accelerated lambda iteration, is presented in detail and practical experiences calculating neutron star atmospheres are reported.

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