Angular momentum transport throughout stellar evolution

Asteroseismology revealed the rotation rate of stellar cores, which is inaccessible to other techniques. Thanks to community efforts, internal rotation rates were measured in thousands of stars ranging from main sequence stars to white dwarfs, and even in exotic stars formed through binary interactions. The first measurements of internal rotation rates in the Sun and red giants revealed the need to revise the theory of angular momentum transport in stellar interiors. Subsequent observations confirmed this issue, indicating that additional physical processes must be incorporated into the stellar evolution theory.

In this talk, I will present the observational data that constrain the physics of angular momentum transport throughout stellar evolution, along with recent theoretical advances aimed at improving its implementation in stellar evolution codes. I will discuss key physical processes that require further study, the observational constraints needed, and how complementary measurements such as asteroseismic envelope rotation rates and internal magnetic fields can help us better understand rotation in stellar interiors. Finally, I will discuss the broader impact of improved angular momentum transport modelling, and its applicability to the study of post-interaction binary stars.