Coronal electron density, temperature and solar spectral irradiance during the solar cycle 23 and 24

TL;DR

This paper introduces the CODET physics-based model to reconstruct and analyze the electron density, temperature, and spectral irradiance in the solar corona during solar cycles 23 and 24, using long-term observational data.

Contribution

The study develops and applies the CODET model to reconstruct coronal plasma parameters and spectral irradiance over extended periods, linking them to magnetic field variations.

Findings

Successful reconstruction of EUV spectral irradiance variability.

Correlation of density and temperature variations with magnetic field changes.

Emission maps consistent with observational data.

Abstract

The plasma parameters such as the electron density and temperature plays a key role in the dynamics of the solar atmosphere. These characteristics are important in solar physics, because they can help to understand the physics in the solar corona. The goal is to reconstruct the electron density and temperature distributions in the solar corona. The relations between emission and plasma parameters in different time scales are studied. We present a physics-based model to reconstruct the density, temperature and emission in the EUV band. This model called CODET is composed of a flux transport model, an extrapolation model, an emission model and an optimization algorithm. The CODET model parameters were constrained by comparing the model's output to the TIMED/SEE record instead of direct observations because it covers a longer time interval than the direct solar observations currently available. The most important results of the current work that the recovery of SSI variability in specific wavelengths in the EUV band, also the variations in density and temperature in large time scale through the solar atmosphere, with the CODET model. The evolution of the electron density and temperature profiles through the solar corona in different layers during the solar cycle 23 and 24, will be presented. The emission maps were obtained and they are in accordance to the observations. Also, the density and temperature maps are related to the variations of the magnetic field in different layers through the solar atmosphere.