Modeling Scattering Polarization for Probing Solar Magnetism

TL;DR

This paper models scattering polarization in the solar atmosphere to improve understanding of solar magnetism, proposing new observational techniques with UV polarimeters for space-based solar diagnostics.

Contribution

It introduces advanced radiative transfer simulations in 3D solar models to predict polarization signals sensitive to magnetic fields, aiding solar magnetic diagnostics.

Findings

Predicted polarization amplitudes in transition region lines.

Identified magnetic sensitivities of scattering polarization signals.

Suggested development of UV polarimeters for space telescopes.

Abstract

This paper considers the problem of modeling the light polarization that emerges from an astrophysical plasma composed of atoms whose excitation state is significantly influenced by the anisotropy of the incident radiation field. In particular, it highlights how radiative transfer simulations in three-dimensional models of the quiet solar atmosphere may help us to probe its thermal and magnetic structure, from the near equilibrium photosphere to the highly non-equilibrium upper chromosphere. The paper finishes with predictions concerning the amplitudes and magnetic sensitivities of the linear polarization signals produced by scattering processes in two transition region lines, which should encourage us to develop UV polarimeters for sounding rockets and space telescopes with the aim of opening up a new diagnostic window in astrophysics.