An Overview of Asteroseismology - May Gade Pedersen
Kavli Institute for Theoretical Physics via YouTube
Overview
Syllabus
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
Taught by
Kavli Institute for Theoretical Physics