Current stellar models are being used in different ways to infer the fundamental properties of stars (mass, radius, age) for Galaxy studies or planetary systems characterization among other fields. These stellar parameters are classically obtained by fitting isochrones on colors or by fitting spectroscopic observables.
With asteroseismology, we can add to the list of observables the global seismic parameters of oscillations and when the signal-to-noise ratio is high enough the individual frequencies of the modes yielding to even more precise stellar parameters.

In the past, seismic observations of the Sun allowed us to improve the physics of the stellar models, for example by reducing the discrepancy between the observed sound speed profile and the modeled one. However, these state-of-the art stellar evolution codes do not include all the physics and need improvements to better reproduce the observations.

In this talk, I will review the different burning topics in the current stellar modeling and I will show how asteroseismology has been and will be providing constraints for improving the physics included in the stellar models.