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An Overview of Asteroseismology - May Gade Pedersen
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- 1 Intro
- 2 Stellar evolution
- 3 What appliance can pierce through the outer layers of a star and test the conditions within?
- 4 Goals of asteroseismology
- 5 Pulsation modes in a star
- 6 Pure inertial modes
- 7 Mode identification: p-modes
- 8 Mode identification: P-g-and mixed modes
- 9 Mode identification: g-modes
- 10 Lightcurves and time bases
- 11 Space telescopes
- 12 Observed core rotation rates
- 13 Cores of RGB and RC stars spin too slowly
- 14 Core rotation rates possibly reconciled
- 15 Age dependence of "core" rotation in B stars
- 16 Observed core vs surface rotation rates
- 17 Current discrepancies with AM predictions
- 18 A star with a slightly faster rotating envelope
- 19 Counter rotation observed in B-type star
- 20 Example sources of internal mixing Microscopie
- 21 Microscopic atomic diffusion needed for A-type star
- 22 Temperature gradient determined from g-modes
- 23 Diverse internal mixing seen in 26 SPB stars
- 24 Signatures of magnetic fields in Red Giants Amplitude suppression
- 25 Main-sequence intermediate mass stars
- 26 Stochastic low-frequency variability
- 27 Discovery of "single" sided pulsators
- 28 Gaia-asteroseismic mass map from red giants
- 29 Take away
