University of Innsbruck, Austria
It has been almost 60 years since the pioneering works of Hayashi, Henyey, and Iben on the evolution of pre-main sequence stars. Several astrophysical research fields, such as asteroseismology, have not yet moved on to a more realistic description of the pre-main sequence evolution, but still rely on these early works.
In this talk, I will introduce the history of classical pre-main sequence models and how we can improve them by modelling accreting protostellar seeds. A comparison between the evolutionary tracks of these accreting protostellar seeds with spectroscopic parameters of pre-main sequence stars allows to put constraints on the constant-accretion rate scenario.
I will also show our results of a linear non-adiabatic pulsation analysis on the resulting models to compare the theoretical and observational instability regions for pre-main sequence δ-Scuti, γ-Doradus, and SPB stars. The locations of known pre-main sequence pulsators and their atmospheric properties derived from high-resolution spectroscopy agree well to our calculated instability regions. I will conclude by discussing the future potential of this state of the art pre-main sequence models.
2021 May 19, 13:30
Online broadcast (Zoom)