Disentangling the Physics of Massive Star Mass Loss After the Main-Sequence
Dylan N. Kee
National Solar Observatory in Hawaii
Understanding the final fates of massive stars, especially the properties of their supernova demises and the compact remnants they leave behind, is deeply entangled with the stellar wind mass loss these stars undergo throughout their lifetimes. Observations show that this mass loss is especially vigorous during the late phases of stellar evolution. However, our theoretical understanding of the physical processes at play in initiating and accelerating stellar winds during this crucial phase is still developing. In this seminar I present recent advances in this area. Specifically, I discuss a first theoretical model for red supergiant mass loss based on turbulent pressure, and first numerical simulations of the winds of hot Wolf-Rayet stars. I conclude by discussing the implications of these recent theoretical advancements in late phase massive star mass loss in both phases for these stars' final fates.
|Date: ||Jeudi, le 9 février 2023|
|Lieu: ||Université de Montréal|
| ||Campus MIL salle A3541|