Magneto-optical effects in the scattering polarization wings of the Ca I resonance line at 4227 angstroms

TL;DR

This paper demonstrates that magneto-optical effects significantly influence the scattering polarization wings of the Ca I 4227 angstrom line, revealing new magnetic sensitivities useful for probing the solar atmosphere's magnetic fields.

Contribution

It shows that magneto-optical terms affect the polarization wings, providing a new method to detect magnetic fields in the lower chromosphere through scattering polarization signals.

Findings

Magneto-optical effects produce sizable signals in U/I wings.

Q/I and U/I wings are sensitive to photospheric magnetic fields.

The study enhances techniques for solar magnetic field diagnostics.

Abstract

The linear polarization pattern produced by scattering processes in the Ca I resonance line at 4227 angstroms is a valuable observable for probing the solar atmosphere. Via the Hanle effect, the very significant Q/I and U/I line-center signals are sensitive to the presence of magnetic fields in the lower chromosphere with strengths between 5 and 125 G, approximately. On the other hand, partial frequency redistribution (PRD) produces sizable signals in the wings of the Q/I profile, which have always been thought to be insensitive to the presence of magnetic fields. Interestingly, novel observations of this line revealed a surprising behavior: fully unexpected signals in the wings of the U/I profile and spatial variability in the wings of both Q/I and U/I. Here we show that the magneto-optical (MO) terms of the Stokes-vector transfer equation produce sizable signals in the wings of U/I and a clear sensitivity of the Q/I and U/I wings to the presence of photospheric magnetic fields with strengths similar to those that produce the Hanle effect in the line core. This radiative transfer investigation on the joint action of scattering processes and the Hanle and Zeeman effects should facilitate the development of more reliable techniques for exploring the magnetism of stellar atmospheres. To this end, we can now exploit the circular polarization produced by the Zeeman effect, the magnetic sensitivity caused by the above-mentioned MO effects in the Q/I and U/I wings, and the Hanle effect in the line core.