Convection, Oscillations and GONNNNG

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The long-term goal of this work is an understanding of the magneto-hydrodynamics ofthe solar surface at scales from granules to sup-granules. Here sophisticated numericalsimulations which include realistic three-dimensional, compressible, magneto-convectionwill be used to model the solar surface and investigate the interaction of convection,magnetic fields, and oscillations. The simulations will be used to interpret observationsfrom GONG, SOHO/MDI, and the Swedish 1m Solar Telescope, to test inversionprocedures, and model the subsurface behavior of solar magneto-convection. Specificobjectives include: 1) To uncover the physical processes that determine the solar surfacestructure through the interaction of convection and magnetic fields on scales fromgranulation to supergranulation. 2) To improve our ability to probe the internal structureof the Sun via helioseismology. 3) To calibrate local helioseismic inversion proceduresfor determining temperatures, flows and magnetic fields near the solar surface. 4) Toinvestigate p-mode physics (dynamic, magnetic and radiative effects on modefrequencies, amplitudes and line asymmetries). 5) To probe the creation, emergence,dispersion and disappearance of magnetic flux in the quiet Sun. And 6) to examine theorigin and maintenance of the magnetic network.The data sets from these simulations will be made available to the community. Thedesign of future solar telescopes will be facilitated through the quantitative informationon observables that will result from this work. These calculations will also improve spaceweather modeling by providing realistic statistical boundary conditions for numericalstudies of the dynamic solar chromosphere and corona.