  The plasma $\beta$ is important to investigate the 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
is to obtain the plasma $\beta$ variations through the solar corona during the
solar cycles 23 and 24. The plasma $\beta$ is reconstructed in different layers
of the solar atmosphere. For this purpose, we use an updated version of COronal
DEnsity and Temperature (CODET) model. In this version, we selected different
features in the solar atmosphere such as Quiet Sun (QS), faculae and Active
Regions (ARs). We calculate the $\beta$ 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 $R_{\odot}$). In the photosphere, we use temperature values
from FALC model to obtain plasma $\beta$ in QS and faculae. Additionally,
variations of the magnetic and kinetic pressure were modelled during the last
solar cycles at coronal heights. Accepted for publication in ApJ.
