Asteroseismology of Sun-like stars and the connexion to the Sun

The Kepler space-borne instrument has been providing high quality photometric lightcurves for distant stars, enabling detailed asteroseismic studies for thousands of stars. Due to this, our understanding of the rotation of Sun-like stars has been significantly improved. There is now clear evidences for an angular momentum transport acting within Sun-like stars and enforcing a weak radial differential rotation (Deheuvels+2014, Deheuvels+2015, Benomar+2015, Nielsen+2017), consistent with helioseismic inferences (e.g. Thompson M., 2003). Kepler data also enabled us to evaluate the latitudinal differential rotation for main-sequence Sun-like stars. This has shown that a vast majority of them are likely to have a slow pole and a faster equator, as it is observed for the Sun (Benomar+2018, Bazot+2019). Although ~30% of the Sun-like stars may show a much stronger latitudinal differential rotation than the Sun, these results suggest that the mechanisms in play in the Sun may not be different than most Sun-like stars in terms of magnetism, activity and dynamo.