1. Summary

2. Two directions in modeling Adopting physical (realistic) models Creating artificial data sets with simplified physics

3. What modelers do Non-linear realistic simulations: 48x48x20 Mm; 50x50x45 Mm –Supergranulation, and other convective scale –realistic artificial data – time-distance Emerging flux: 23 Mm, very close to the surface (f-modes ?) High-resolution: 6Mm, 6 km resolution Global simulations: how to couple to near-surface simulations (SSW maps); narrow the gap to the dynamo models. Links to HMI –Meridional circulation –NS lanes –Latitudinal variations –Thermal/velocity/magnetic correlations –Torsional oscillations Artificial data –Acoustic waves on sphere –Acoustic waves in box –Full Navier-Stokes

4. What observers want Time-distance –Improve power distribution –Magnetic field – sunspot areas ! –Large-scale flows –Sensitivity kernels from simulations – testing approximations Rings –Line profile modeling - non-Lorentzian –20-200 Mm depth 16 Mm, 8-24 hours –Complicated flow fields –Non-uniform amplitude distribution due to magnetic field Holography –Acoustic emission sources – high frequencies –Modeling the far-side signal –Artificial data + wave physics understanding

5. Wave interaction with sunspots Courtesy E.Khomenko Need to continue work of K.Julien, C.Rosenthal, 2000