Numerical Methods in Polarized Radiative Transfer

Details Numerical Methods in Polarized Radiative Transfer Numerical Methods in Polarized Radiative Transfer

Mar 1996

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996soph..164..103r&link_type=abstract

Solar Physics, Volume 164, Issue 1-2, pp. 103-116

Physics

2

Polarization, Radiative Transfer, Magnetic Fields, Wavelets

Scientific paper

This paper looks at three aspects of numerical methods for solving polarized radiative transfer problems associated with spectral line formation in the presence of a magnetic field. First we prove “Murphy's law for Stokes evolution operators” which is the basis of the efficient algorithm used in the SPSR software package to compute the Stokes line depression contribution functions. Then we use a two-stream model to explain the efficacy of the field-free method in which the non-LTE line source function in a uniform magnetic field is approximated by the source function neglecting the magnetic field. Finally we introduce a totally new and computationally efficient approach to solving non-LTE problems based on a method of sparsely representing integral operators using wavelets. As an illustration, the wavelet method is used to solve the source function integral equation for a two-level atomic model in a finite atmosphere with coherent scattering, ignoring polarization.

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