Formation of the Mg II h and k polarization profiles in a solar plage model and their suitability to infer magnetic fields

TL;DR

This study investigates the formation of Mg II h and k polarization profiles in a solar plage model, assessing their effectiveness for magnetic field inference through radiative transfer simulations aligned with CLASP2 observations.

Contribution

It provides a detailed analysis of the polarization profiles' formation and demonstrates improved magnetic field diagnostics using selective weak field approximation techniques.

Findings

Profiles show strong asymmetries complicating weak field approximation

Selective fitting of spectral regions improves magnetic field retrieval

Profiles formed in regions with velocity and magnetic gradients

Abstract

The Mg II h and k lines are among the strongest in the near-ultraviolet solar spectrum and their line core originates in the upper chromosphere, just below the transition region. Consequently, they have become one of the main targets for investigating the magnetism of the upper solar atmosphere. The recent CLASP2 mission obtained unprecedented spectropolarimetric data of these lines in an active region plage, which have already been used to infer the longitudinal component of the magnetic field by applying the weak field approximation. In this paper, we aim at improving our understanding of the diagnostic capabilities of these lines by studying the emergent Stokes profiles resulting from radiative transfer calculations in a radiative magneto-hydrodynamic (rMHD) time-dependent model representative of a solar plage. To this end, we create a synthetic observation with temporal and spatial resolutions similar to those of CLASP2. We find strong asymmetries in the circular polarization synthetic profiles which considerably complicate the application of the weak field approximation. We demonstrate that the selective application of the weak field approximation to fit different spectral regions in the profile allows to retrieve information about the longitudinal component of the magnetic field at different regions of the model atmosphere, even when the circular polarization profiles are not anti-symmetric and are formed in the presence of strong velocity and magnetic field gradients.