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The plasma parameters such as the electron density and temperature plays akey role in the dynamics of the solar atmosphere. These characteristics areimportant in solar physics, because they can help to understand the physics inthe solar corona. The goal is to reconstruct the electron density andtemperature distributions in the solar corona. The relations between emissionand plasma parameters in different time scales are studied. We present aphysics-based model to reconstruct the density, temperature and emission in theEUV band. This model called CODET is composed of a flux transport model, anextrapolation model, an emission model and an optimization algorithm. The CODETmodel parameters were constrained by comparing the model's output to theTIMED/SEE record instead of direct observations because it covers a longer timeinterval than the direct solar observations currently available. The mostimportant results of the current work that the recovery of SSI variability inspecific wavelengths in the EUV band, also the variations in density andtemperature in large time scale through the solar atmosphere, with the CODETmodel. The evolution of the electron density and temperature profiles throughthe solar corona in different layers during the solar cycle 23 and 24, will bepresented. The emission maps were obtained and they are in accordance to theobservations. Also, the density and temperature maps are related to thevariations of the magnetic field in different layers through the solaratmosphere.

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