Remote Sensing of Chromospheric Magnetic Fields via the Hanle and Zeeman Effects

TL;DR

This paper discusses how polarization signals in chromospheric spectral lines, influenced by Hanle and Zeeman effects, can be used to empirically study weak magnetic fields in the solar chromosphere, advancing spectropolarimetric techniques.

Contribution

It introduces a physical interpretation of polarization signals caused by atomic polarization and dichroism, enhancing understanding of chromospheric magnetic fields beyond the Zeeman effect.

Findings

Linear polarization Q and U arise from atomic polarization in metastable levels.

Horizontal magnetic fields in the gauss range can produce significant polarization signals.

Recent observational and theoretical advances improve magnetic field diagnostics in the solar atmosphere.

Abstract

The only way to obtain reliable empirical information on the intensity and topology of the weak magnetic fields of the quiet solar chromosphere is via the measurement and rigorous physical interpretation of polarization signals in chromospheric spectral lines. The observed Stokes profiles reported here are due to the Hanle and Zeeman effects operating in a weakly magnetized plasma that is in a state far from local thermodynamic equilibrium. The physical origin of their enigmatic linear polarization Q and U components is the existence of atomic polarization in their metastable lower-levels, which permits the action of a dichroism mechanism that has nothing to do with the transverse Zeeman effect. It is also pointed out that the population imbalances and coherences among the Zeeman sublevels of such long-lived atomic levels can survive in the presence of horizontal magnetic fields having intensities in the gauss range, and produce significant polarization signals. Finally, it is shown how the most recent developments in the observation and theoretical modelling of weak polarization signals are facilitating fundamental new advances in our ability to investigate the magnetism of the outer solar atmosphere via spectropolarimetry.