The Formation of Polarized Lines: Allowance for the Hanle Effect

Details The Formation of Polarized Lines: Allowance for the Hanle Effect The Formation of Polarized Lines: Allowance for the Hanle Effect

Dec 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001arep...45..960g&link_type=abstract

Astronomy Reports, Volume 45, Issue 12, December 2001, pp.960-966

Astronomy and Astrophysics

Astronomy

Scientific paper

The paper formulates the standard theory for the transport of polarized radiation in the presence of resonance scattering in an atmosphere with a weak magnetic field, so that the Zeeman splitting is small compared to the Doppler line width. For an atmosphere with conservative scattering, this reduces to the Milne problem, which consists of computing a polarized radiation field in a medium with sources lying in infinitely deep layers. In the approximation of complete frequency redistribution, the problem reduces to solving a Wiener-Hopf integral equation for a (6×6)-matrix source function. Asymptotic and numerical solutions for the standard problem are obtained, including solutions for the Milne problem, for the case of a Doppler absorption profile. The line polarization profiles for the emergent flux at various angular distances from the disk center are derived, and the dependence of the limiting degree of polarization (at the line center at the disk edge) on the direction of the magnetic field is computed. For nearly conservative scattering with photon destruction probability ɛ≪1, the limiting degree of polarization varies with ɛ in accordance with a simple empirical law similar to that found earlier for a medium with zero magnetic field.

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