Three-dimensional simulations of scattering polarization and the Hanle effect in MHD chromospheric models

TL;DR

This paper reviews recent advances in 3D NLTE radiative transfer simulations of scattering polarization and the Hanle effect in magnetohydrodynamic models of the solar atmosphere, aiding interpretation of spectropolarimetric data.

Contribution

It provides an overview of recent progress in 3D NLTE spectral line synthesis using the PORTA code in realistic MHD chromospheric models.

Findings

Enhanced understanding of scattering polarization in 3D MHD models

Improved interpretation of solar spectropolarimetric observations

Advancements in radiative transfer modeling techniques

Abstract

Scattering line polarization and the Hanle effect are among the most important mechanisms for diagnostics of the solar and stellar atmospheres. The fact that real stellar atmospheres are horizontally inhomogeneous makes the spectral synthesis and interpretation very challenging because the effect of thermodynamic fluctuations on spectral line polarization is entangled with the action of magnetic fields. This applies to the spatially resolved as well as to the averaged spectra. The necessary step towards the interpretation of such spectra is to study the line formation in sufficiently realistic 3D MHD models and comparison of the synthetic spectra with observations. This paper gives an overview of recent progress in the field of 3D NLTE synthesis of polarized spectral lines resulting from investigations with the radiative transfer code PORTA.