New Approach to the Solar Evolutionary Model with Helioseismic Constraints

l The traditional procedure for modeling solar evolution is to perform a calibration. It is a process of adjusting the convection parameter alpha, and hydrogen initial abundance X-0, to obtain a model with given radius and luminosity at a specified age. Helioseismology provides rather precise determinations of the solar convection boundary position R-cz, and helium content in the envelope Y-cz. Modern standard models of the Sun have R-cz and Y-cz close to the helioseismic values. However certain investigations connected with eigenfrequency analysis require solar models with exact values of Ycz and especially R-cz. This work proposes a method to calculate models with specified convection zone parameters. Target calibration values can be chosen from the set of R-cz, Y-cz, Z(cz) and mass parameter M-75 (mass coordinate at radius 0.75 R-circle dot). The method is based on local and global opacity modifications. Global modification allows the calibration of Y-cz, a local change in the radiative zone which mainly affects the specific entropy in the solar convection zone boundary S-cz. Convection zone depth depends on Y-cz, Z(cz), M-75 or can be independently adjusted via a local correction.