What we know and do not know about neutrino production in stars

This review summarizes the necessary ingredients for determining the neutrino production rates in stars. Then the case of the Sun is studying. A detailed comparison between solar neutrino predictions and each neutrino detection shows the interest of the seismic model versus standard model. After the determination of θ12, Δm212 and the inclusion of electronic neutrino transformation, the global agreement is a noticeable success with nevertheless some identified questions. The second part of the review is dedicated to the important lacks in solar and stellar modelling and to the way we are presently attacking the different problems. Such situation encourages to pursue the effort on stellar neutrino detections and neutrino predictions, astrophysics modelling with evident consequences for stellar evolution, supernovae explosion and neutrino properties.