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In this work we use the semi-empirical atmospheric modeling method to obtainthe chro-mospheric temperature, pressure, density and magnetic fielddistribution versus height in the K2 primary component of the RS CVn binarysystem HR 7428. While temperature, pressure, density are the standard output ofthe semi-empirical modeling technique, the chromospheric magnetic fieldestimation versus height comes from considering the possibility of notim-posing hydrostatic equilibrium in the semi-empirical computation. Thestability of the best non-hydrostatic equilibrium model, implies the presenceof an additive (toward the center of the star) pressure, that decreases instrength from the base of the chromosphere toward the outer layers.Interpreting the additive pressure as magnetic pressure we estimated a magneticfield intensity of about 500 gauss at the base of the chromosphere.

Estimating the chromospheric magnetic field from a revised NLTE modeling: the case of HR7428