An Overview of Asteroseismology - May Gade Pedersen

Explore an in-depth overview of asteroseismology in this 58-minute conference talk from the Transport in Stellar Interiors Conference at KITP. Delve into the latest advancements in observational data, including TESS and spectroscopic studies, and their impact on our understanding of transport processes in stellar interiors. Examine various aspects of stellar physics, including heat transfer, chemical element distribution, and angular momentum. Discover how pulsation modes in stars can be used to probe their internal conditions, and learn about the different types of modes such as p-modes, g-modes, and mixed modes. Investigate the observed core rotation rates in various types of stars and the current discrepancies with angular momentum predictions. Explore the diverse internal mixing processes observed in stars and their implications for stellar evolution. Gain insights into the signatures of magnetic fields in red giants and the discovery of "single-sided" pulsators. Conclude with a look at the Gaia-asteroseismic mass map from red giants and key takeaways from this comprehensive exploration of asteroseismology.

Intro
Stellar evolution
What appliance can pierce through the outer layers of a star and test the conditions within?
Goals of asteroseismology
Pulsation modes in a star
Pure inertial modes
Mode identification: p-modes
Mode identification: P-g-and mixed modes
Mode identification: g-modes
Lightcurves and time bases
Space telescopes
Observed core rotation rates
Cores of RGB and RC stars spin too slowly
Core rotation rates possibly reconciled
Age dependence of "core" rotation in B stars
Observed core vs surface rotation rates
Current discrepancies with AM predictions
A star with a slightly faster rotating envelope
Counter rotation observed in B-type star
Example sources of internal mixing Microscopie
Microscopic atomic diffusion needed for A-type star
Temperature gradient determined from g-modes
Diverse internal mixing seen in 26 SPB stars
Signatures of magnetic fields in Red Giants Amplitude suppression
Main-sequence intermediate mass stars
Stochastic low-frequency variability
Discovery of "single" sided pulsators
Gaia-asteroseismic mass map from red giants
Take away