1. Simulations of Solar Convection Zone Nagi N. Mansour

2. Goals Provide numerical simulation models for interpretation of SDO data Develop understanding of physical mechanisms in the convection zone and links to the atmosphere Provide simulation data for testing and developing data analyses tools

3. Targets Solar turbulent convection Tachocline Upper convective boundary layer Supergranulation Granulation and wave excitation Wave propagation Magnetoconvection

4. HMI Science Analysis Plan Magnetic Shear Tachocline Differential Rotation Meridional Circulation Near-Surface Shear Layer Activity Complexes Active Regions Sunspots Irradiance Variations Flare Magnetic Configuration Flux Emergence Magnetic Carpet Coronal energetics Large-scale Coronal Fields Solar Wind Far-side Activity Evolution Predicting A-R Emergence IMF Bs Events Brightness Images Global Helioseismology Processing Local Helioseismology Processing Version 1.0w Filtergrams Line-of-sight Magnetograms Vector Magnetograms Doppler Velocity Continuum Brightness Line-of-Sight Magnetic Field Maps Coronal magnetic Field Extrapolations Coronal and Solar wind models Far-side activity index Deep-focus v and c s maps (0-200Mm) High-resolution v and c s maps (0-30Mm) Carrington synoptic v and c s maps (0-30Mm) Full-disk velocity, v(r,Θ,Φ), And sound speed, c s (r,Θ,Φ), Maps (0-30Mm) Internal sound speed, c s (r,Θ) (0<r<R) Internal rotation Ω(r,Θ) (0<r<R) Vector Magnetic Field Maps Science Objective Data Product Processing Observables HMI Data

5. Approach Large-scale 3D simulations: –Fully compressible MHD equations –Inelastic approximation –Realistic thermodynamics –Radiative energy transport Data assimilation and Inverse Modeling

6. Tools Fully compressible MHD equations –Three-Dimensional code (TVD scheme) with realistic equation of state (S. Ustyugov) –High order finite difference LES code with MHD, real gas, radiation and subgrid scale models (A. Wray) –Initiated contact with R. Stein (MSU)

7. Tools Inelastic approximation –Slab geometry with SGS model (M. Kirkpatrick) –Initiated collaboration with Colorado Research Ass./UC Boulder/Stanford U./ARC Spherical Code+LES

8. Resources NASA Supercomputing facility: –SGI 1,024-processor Origin 3000 –SGI 512-processor Origin 3000 –SGI 256-processor Origin –32-processor Cray SV1e –SGI and Sun workstations –600 terabytes online/nearline data storage Stanford SDO/HMI group

9. Development plan Compressible MHD: –Implement SGS and radiation models into the Stein/Nordland code –Data Assimilation –Name the Code and make it available as a Community code under CCMC (Community Coordinated Modeling Center) SIMULATION

10. Development plan Inelastic Code: –(ASH & HYPE) + SGS –Data Assimilation –Make codes available under CCMC SIMULATION

11. Development plan Using data to develop understanding/models –Inverse Modeling UiUjUiUj ?

12. Collaborations Sasha Kosovichev (SDO/HMI) [GURU] Center for Turbulence Research Alan Wray Michael Rogers Sergey Ustyugov Robert Stein (MSU) Colorado Research Ass.: –M. Miesch –J. Werne –T. Lund –K. Julien ( U. Colorado Boulder)

13. Requirements Support for the scientific teams: –CS under full cost accounting –University/Industry science Support of High-End Computing by NASA: –Compute cycles –Formulate IT requirements: Grid Viz. tools Analyses tools