Mg ii h&k spectra of an enhanced network region simulated with the MURaM-ChE code. Results using 1.5D synthesis

TL;DR

This study uses advanced 1.5D radiative transfer modeling with the MURaM-ChE code to simulate Mg ii h&k spectra in an enhanced solar network region, comparing results with IRIS observations to understand line broadening mechanisms.

Contribution

It introduces a novel 1.5D synthesis approach with the MURaM-ChE code for modeling Mg ii lines in a realistic solar atmosphere, improving understanding of line broadening.

Findings

Synthetic line widths are close to observations but slightly narrower.

Chromospheric velocities are key to line broadening.

Discrepancies in peak intensities may be due to magnetic flux and modeling limitations.

Abstract

The Mg ii h&k lines are key diagnostics of the solar chromosphere. They are sensitive to the temperature, density, and non-thermal velocities in the chromosphere. The average Mg ii h&k line profiles arising from previous 3D chromospheric simulations are too narrow. We study the formation and properties of the Mg ii h&k lines in a model atmosphere. We also compare the average spectrum, peak intensity, and peak separation of Mg ii k with a representative observation taken by IRIS. We use a model based on the recently developed non-equilibrium version of the radiative magneto-hydrodynamics code MURaM, in combination with forward modeling using the radiative transfer code RH1.5D to obtain synthetic spectra. Our model resembles an enhanced network region created by using an evolved MURaM quiet sun simulation and adding a similar imposed large-scale bipolar magnetic field as in the public Bifrost snapshot of a bipolar magnetic feature. The line width and the peak separation of the spatially averaged spectrum of the Mg ii h&k lines from the MURaM simulation are close to a representative observation from the quiet sun which also includes network fields. However, we find the synthesized line width to be still slightly narrower than in the observation. We find that velocities in the chromosphere play a dominant role in the broadening of the spectral lines. While the average synthetic spectrum also shows a good match with the observations in the pseudo continuum between the two emission lines, the peak intensities are higher in the modeled spectrum. This discrepancy may partly be due to the larger magnetic flux density in the simulation than in the considered observations but also due to the 1.5D radiative transfer approximation. Our findings show that strong maximum velocity differences or turbulent velocities in the chromosphere are necessary to reproduce the observed line widths.