Generation of Artificial Data in Support of SDO-HMI Nagi N. Mansour, NASA ARC Alan Wray, NASA ARC Thomas Hartlep, Stanford CTR Alexander Kosovichev, Stanford HEPL Thomas Duvall, NASA GSFC Mark Miesch, UCAR

Two efforts in progress: (1)Direct simulation of wave propagation in solar interior (2)Large-eddy simulation of the near-surface convection zone

Random forcing Damping Layer above Surface Wave equation Equations Direct Simulation of Wave Propagation in the Solar Interior

Spherical harmonics, and Basis-Spline in radial direction Resolution in all directions adjustable with r Treatment of coordinate singularity by enforcing regularity condition at the center Non-reflecting boundary by means of a damping layer at the top Temporally random forcing of each spherical harmonics mode Numerical Method Example of B-Splines

Oscillation Power Spectra radial-symmetric Sound Speed of a Standard Solar Model with gravity term without gravity term

StellarBox Rectangular geometry 50  50  43 Mm Compressible, radiation-hydro equations LTE radiation, 14 ray angular quadrature Non-ideal (tabular) EOS; tabular, binned opacity 4th order Padé derivatives 3rd (or 4th) order Runge-Kutta in time No-penetration, hydrostatic-pressure b.c.’s MPI parallelization

StellarBox MPI code Scaling results on Columbia

Current status 500  500  500 on 100 processors (typically) ~7-8 hour runs steps/run Also used on brown dwarf stars

Vertical velocity in an x-z plane

Enstrophy ( |  | 2 ) in an x-z plane