A new generation of evolutionary and seismic solar models

The Sun is the most observed star in the Universe. Thanks to this privileged status, it plays a key calibrator role for stellar physics, acting as a laboratory to test fundamental physical ingredients used in theoretical computations. Therefore, any re nement of the recipe of solar models will impact the ingredients for all models of solar-type stars. Following the revision of the solar abundances by Asplund and collaborators in 2005, con rmed in 2009, 2015 and 2021, the standard recipe of solar models has been put under question regarding both microscopic and macroscopic ingredients. In this work, we will present results of new generations of both solar evolutionary and seismic models. We will show how evolutionary models taking into account the e ects of rotation and magnetic elds can reproduce both the internal rotation, the lithium surface abundance and the helium abundance in the convective zone of the Sun. Furthermore, we will present a new approach to compute seismic solar models from iterative Ledoux discriminant inversions. We will show how such seismic models can be used to gain insights on the temperature gradient close to the base of the convective zone, where the robustness of opacity tables has been questioned. Combining both approaches will thus provide us with key constraints on the required revision of physical ingredients to solve the long lasting solar modeling problem that followed the abundance revision in the early 2000s.