Solar structure models

The Sun is a unique object in stellar evolution due to our unprecedent insight on its internal processes. We will illustrate in this review how the transition between a static vision to a more dynamical vision modifies the addressing questions on the solar radiative zone. Neutrinos and acoustic modes have first scrutinized the microscopic properties of the solar radiative plasma. Today, stimulated by the internal rotation profile determination, new questions emerge on the angular momentum transport by rotation, internal waves and on the role of magnetic fields to get access to the dynamical motions of this important region of the Sun. We will give some examples which demonstrate that the Sun is not yet under control.