Scattering Polarization and Hanle Effect in Stellar Atmospheres with Horizontal Inhomogeneities

TL;DR

This paper develops a method to analyze how horizontal inhomogeneities and magnetic fields in stellar atmospheres affect scattering polarization and the Hanle effect, providing insights and benchmarks for multidimensional radiative transfer modeling.

Contribution

It introduces a linearized, harmonic analysis-based method to solve polarized radiative transfer in atmospheres with weak horizontal fluctuations, accounting for magnetic field effects.

Findings

Horizontal inhomogeneities alter polarization amplitudes.

Vertical magnetic fields can modify line polarization due to inhomogeneities.

Forward scattering polarization can occur without inclined magnetic fields.

Abstract

Scattering of light from an anisotropic source produces linear polarization in spectral lines and the continuum. In the outer layers of a stellar atmosphere the anisotropy of the radiation field is typically dominated by the radiation escaping away, but local horizontal fluctuations of the physical conditions may also contribute, distorting the illumination and hence, the polarization pattern. Additionally, a magnetic field may perturb and modify the line scattering polarization signals through the Hanle effect. Here, we study such symmetry-breaking effects. We develop a method to solve the transfer of polarized radiation in a scattering atmosphere with weak horizontal fluctuations of the opacity and source functions. It comprises linearization (small opacity fluctuations are assumed), reduction to a quasi-planeparallel problem through harmonic analysis, and numerical solution by generalized standard techniques. We apply this method to study scattering polarization in atmospheres with horizontal fluctuations in the Planck function and opacity. We derive several very general results and constraints from considerations on the symmetries and dimensionality of the problem, and we give explicit solutions of a few illustrative problems of especial interest. For example, we show (a) how the amplitudes of the fractional linear polarization signals change when considering increasingly smaller horizontal atmospheric inhomogeneities, (b) that in the presence of such inhomogeneities even a vertical magnetic field may modify the scattering line polarization, and (c) that forward scattering polarization may be produced without the need of an inclined magnetic field. These results are important to understand the physics of the problem and as benchmarks for multidimensional radiative transfer codes.