The plasma β is important in the investigation of interchanging roles of plasma and magnetic pressure in the solar atmosphere. It can help to describe features over the photosphere and their changes at different heights. The goal of this paper is to obtain the plasma β variations through the solar corona during solar cycles 23 and 24. The plasma β is reconstructed in different layers of the solar atmosphere. For this purpose, we use an updated version of the COronal DEnsity and Temperature model. In this version we selected different features in the solar atmosphere such as quiet-Sun (QS), faculae, and active regions. We calculate the β variations at different layers in the solar corona (R = 1.14, 1.19, 1.23, 1.28, 1.34, 1.40, 1.46, 1.53, 1.61, 1.74, 1.79, 1.84, and 1.90 R o). In the photosphere we use temperature values from the FALC model to obtain plasma β in QS and faculae. Additionally, variations of the magnetic and kinetic pressure were modeled during the last solar cycles at coronal heights.
- Sun: magnetic fields
- Sun: photosphere