1. Travis Metcalfe (NCAR) Asteroseismology with the Kepler Mission We are the stars which sing, We sing with our light; We are the birds of fire, We fly over the sky. SONG OF THE STARS Algonquin Mythology

2. Why is asteroseismology important to the primary science goal of Kepler? Transit only gives radius of planet relative to the unknown stellar radius Asteroseismology will measure the stellar radius with a precision of 2-3%

3. Why is asteroseismology important to the primary science goal of Kepler? Transit only gives radius of planet relative to the unknown stellar radius Asteroseismology will measure the stellar radius with a precision of 2-3%

4. Kepler mission overview NASA mission currently scheduled for launch in mid-February 2009 105 square degrees just above galactic plane in the constellation Cygnus Single field for 4-6 years, 100,000 stars 30 minute sampling, 512 at 1 minute

5. Surface differential rotation Three seasons of precise MOST photometry for the solar-type star  1 Ceti Latitudinal differential rotation pattern has same functional form as Sun Kepler will obtain similar rotation measurements for 10 5 solar-type stars Walker et al. (2007) Ca HK period

6. Stellar density and age Large frequency spacing scales with average density of the star Small frequency spacing sensitive to interior gradients, proxy for age Probe evolution of activity and rotation as a function of stellar mass and radius Christensen-Dalsgaard (2004) Elsworth & Thompson (2004)

7. WIRE 50-day time series of  Cen A has resolved the rotational splitting Splitting as a function of radial order can indirectly probe differential rotation Even low-degree modes allow rough inversions of the inner 30% of radius Gough & Kosovichev (1993) Radial differential rotation Fletcher et al. (2006)

8. Convection zone depth Expected seismic signal from a CoRoT 5-month observation of HD 49933 Second differences (  2 ) measure deviations from even frequency spacing Base of the convection zone and He ionization create oscillatory signals Baglin et al. (2006)

9. Solar p-mode shifts first detected in 1990, depend on frequency and degree Even the lowest degree solar p-modes are shifted by the magnetic cycle Unique constraints on the mechanism could come from asteroseismology Oscillations and magnetic cycles Libbrecht & Woodard (1990) Salabert et al. (2004)

10. Solar p-mode shifts show spread with degree and frequency dependence Normalizing shifts by our parametrization removes most of the dependencies Kepler will document similar shifts in hundreds of solar-type stars Cycle-induced frequency shifts Metcalfe et al. (2007)

11. Stellar modeling pipeline Genetic algorithm probes a broad range of possible model parameters 0.75 < M star < 1.75 0.002 < Z init < 0.05 0.22 < Y init < 0.32 1.0 <  mlt < 3.0 Finds optimal balance between asteroseismic and other constraints

12. Application to BiSON data Fit to 36 frequencies with l = 0-2 and constraints on temperature, luminosity Matches frequencies with scaled surface correction better than 0.6  Hz r.m.s. Temperature and age within +0.1%, luminosity and radius within +0.4%

13. TeraGrid portal Web interface to specify observations with errors, or upload as a text file Specify parameter values to run one instance of the model, results archived Source code available for those with access to large cluster or supercomputer

14. Summary Kepler needs asteroseismology to determine the absolute sizes of any potentially habitable Earth- like planets that may be discovered. The mission will yield a variety of data to calibrate dynamo models, sampling many different sets of physical conditions and evolutionary phases. A uniform analysis of the asteroseismic data will help minimize the systematic errors, facilitated by a TeraGrid-based community modeling tool.