Small-scale chromospheric spectropolarimetric observables in the internetwork from a 3D radiative MHD model

TL;DR

This paper uses a high-resolution 3D radiative MHD model to simulate and interpret small-scale chromospheric spectropolarimetric signals, aiding the analysis of upcoming solar observations.

Contribution

It introduces detailed synthetic spectropolarimetric profiles from a realistic 3D MHD model, enhancing the understanding of chromospheric magnetic observables.

Findings

Doppler shift compensation is essential for accurate magnetic field diagnostics.

Synthetic profiles match expected observables from DKIST and IRIS.

Insights aid interpretation of future high-resolution solar observations.

Abstract

The presence of the magnetic field is critical to transport energy through the solar atmosphere. The new generation of telescopes will provide new insight into how the magnetic field arrives into the chromosphere and its role in the energy balance of the solar atmosphere. We have used a 3D radiative MHD numerical model of the solar atmosphere with high spatial resolution (4~km) calculated with the Bifrost code. This code solves the full MHD equations with non-grey and non-LTE radiative transfer and thermal conduction along magnetic field lines. The model shows how the lower chromosphere in the internetwork, a region dominated by magneto-acoustic shocks and where plasma beta is greater than 1, is able to generate magnetic field in-situ Martinez-Sykora et al 2019. We have synthesized full-polarimetric Stokes profiles from this model for several spectral lines formed in the photosphere and the chromosphere. These synthetic profiles illustrate the types of observables expected from DKIST and IRIS. Our work provides insight into how to interpret observations from these observatories. We find that in order to discern the chromospheric magnetic observables it is crucial to compensate for Doppler shift rather than use fix wavelength range.