Parameters of the Solar Convection Zone in Evolutionary and Seismic Models

Three alternative approaches in evaluating of the entropy of the adiabatic part of the solar convection zone are compared. 1. Entropy as a parameter of solar structure The speciic entropy (s) and the helium abundance (Y), chief parameters of the solar convection zone, are still poorly determined. They are principal characteristics of the equation of state (EOS hereafter), whereas others apparent to be signiicant EOS's features can be rarely characterized in a simple way (e.g. nonideality deviations). We focus on the speciic entropy, which is "implicitly" presented in a wide range of solar studies. Thus the evolutionary calibration of a convec-tion parameter appears to be anything else but calibration of the entropy. Entropy deenes (T ?) proole of the adiabatic convection zone, but together with surface conditions it accurately determines the mechanical structure ((r), m(r)) too. A direct way to calibrate the entropy is adequate modelling of the superadiabatic convection and nding the jump of the entropy between the atmosphere and adiabatic layers. On the other hand, one should equalize the entropy jump before compare of diierent convection theories.