Stokes profile analysis and vector magnetic fields. II - Formal numerical solutions of the Stokes transfer equations

Details Stokes profile analysis and vector magnetic fields. II - Formal numerical solutions of the Stokes transfer equations Stokes profile analysis and vector magnetic fields. II - Formal numerical solutions of the Stokes transfer equations

Apr 1989

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1989apj...339.1093r&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 339, April 15, 1989, p. 1093-1106. Research supported by the High Altitude

Astronomy and Astrophysics

Astrophysics

112

Radiative Transfer, Solar Magnetic Field, Solar Spectra, Zeeman Effect, Calcium, Differential Equations, K Lines, Solar Atmosphere, Stokes Law Of Radiation, Thermodynamic Equilibrium

Scientific paper

Two numerical methods for formal integration of the Stokes transfer equations for line formation in a strong magnetic field were tested by computing Stokes profiles for a Zeeman triplet in a Milne-Eddington model atmosphere, and for the anomalously split Ca II K line in a realistic solar model. The first method is a Feautrier (1964) type method, in which the equations are written in second-order form and solved by finite-differences. The second method is a new solution called DELO, in which an integral equation for the Stokes vector is formulated in terms of the lambda operator (LO) associated with the diagonal elements (DE) of the absorption matrix. It is shown that the DELO method is faster and more accurate than the Feautrier method, and that both methods are more efficient than the Runge-Kutta integration method.

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