# Observations of the solar chromosphere with ALMA and comparison with theoretical models

## TL;DR

This paper uses ALMA solar observations at 1.21 mm to analyze the solar chromosphere, comparing observational data with modified atmospheric models to enhance understanding of this dynamic solar layer.

## Contribution

It combines high-resolution ALMA observations with modified FAL atmospheric models to improve the understanding of the solar chromosphere's structure and dynamics.

## Key findings

- Agreement between observations and models enhances understanding of chromospheric features
- Identification of discrepancies leading to improved atmospheric modeling
- Insights into the temperature and density structure of the chromosphere

## Abstract

In this work we use solar observations with the ALMA radio telescope at the wavelength of 1.21 mm. The aim of the analysis is to improve understanding of the solar chromosphere, a dynamic layer in the solar atmosphere between the photosphere and corona. The study has an observational and a modeling part. In the observational part full-disc solar images are analyzed. Based on a modified FAL atmospheric model, radiation models for various observed solar structures are developed. Finally, the observational and modeling results are compared and discussed.