A Practical Introduction to Stellar Nonradial Oscillations (i) Rich Townsend University of Delaware ESO Chile ̶ November 2006 TexPoint fonts used in EMF.

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Presentation transcript:

A Practical Introduction to Stellar Nonradial Oscillations (i) Rich Townsend University of Delaware ESO Chile ̶ November 2006 TexPoint fonts used in EMF. Read the TexPoint manual before you delete this box.: A AAA

Overview Historical Perspective –Radial pulsators –Nonradial pulsators Waves in stars Global oscillations Surface variations Rotation effects Driving mechanisms

p-mode Surface Variations

g-mode Surface Variations

p modes vs. g modes

Carnot Cycle

Excitation Mechanisms Add heat when temperature is high Remove heat when temperature is low Mechanisms: –κ : opacity –ε : nuclear energy –δ : superadiabatic stratification –γ : ionization

OPAL / OP Opacities

5 M ¯ model

WN model

Brown Dwarf model

Asteroseismology Compare observations against models –Frequencies –Multi-color light curve Amplitudes Phases –Spectroscopy Line-profile variations Mean profiles

Frequencies

Photometric Amplitudes ℓ = 1 ℓ = 2 ℓ = 3

Line-Profile Variations

lpv: Time-Series

Modeling Photometric –Semi-analytical Spectroscopic –Semi-analytical Moments TVS –Numerical BRUCE/KYLIE PULSTAR

Photometric Modeling Stamford & Watson (1981) Semi-analytical formula for flux changes

Photometry of SPB stars

Spectroscopic Modeling Represent stellar surface with mesh Perturb mesh with pulsation(s) Rasterize mesh Synthesize spectra for each pixel Combine spectra

Spectral Synthesis For each pixel: –Teff –log g –V –  Interpolate spectrum in intensity grid

Pulsation & Rotation Coriolis force becomes significant when Ω/ω > 0.5 Pulsation confined within equatorial waveguide New formula –Townsend (2003) –Extends Dziembowski (1977) –Low-frequency (SPBs)

Effects of Rotation Townsend (2003)