Stellar Magnetism across the HR diagram: origins and detectability
Kyle Auguston
CEA Paris-Saclay



Many stars exhibit magnetic features throughout their evolution, from nascent proto-stars to evolved giants. Magnetic fields combined with rotation play critical roles in the internal transport of angular momentum and chemical species. They also play a role in the loss of mass and angular momentum from winds. It is therefore of great use in many corners of astrophysics to pin down the nature of the magnetic fields in the star and how it interacts with rotation and convection to drive dynamo action to sustain itself and the nature of the instabilities that it can trigger. Here we will review the current paradigms in the study of the magnetism of our nearest star as well as the processes active in other stars that lead to their detected magnetic fields. Specifically, we will look at how convective dynamics lead to the cyclic magnetic dynamos in low-mass main-sequence stars (M- to F-type) and what the implications are for fossil field-convective dynamo interactions of higher-mass main-sequence stars (A- to O-type).