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Advancements in MHD Modeling for HMI: Insights from the Stanford Meeting

The 2009 HMI/AIA science team meeting at Stanford focused on the development of MHD models to study solar magnetic field dynamics. Key discussions included the use of magnetic field data and plasma parameters as input for extrapolating 3D magnetic and plasma structures, with outputs such as open/closed coronal field structures and flow speed estimations. Emphasis was placed on achieving quasi-steady states through a polytropic equation of state and utilizing advanced computational capabilities for real-time data processing in research on solar phenomena.

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Advancements in MHD Modeling for HMI: Insights from the Stanford Meeting

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  1. HMI/AIA science team meeting Sep. 8 -- 11, 2009 Stanford, CA MHD model in HMI pipeline

  2. MHD models • Input : as initial & boundary values, the magnetic field data, in various formats and cadences, (and plasma parameters from observations) • Output : theoretical determination / extrapolation of • 3D magnetic and plasma structures, above the photosphere, and in interplanetary space including the high heliographic latitude region, • Temporal evolutions, and • Views from various directions • MHD models can give unobservables • MHD models can give observables by independent observations

  3. Input, (quasi-) real-time base • EOF (experiment operations facility) preliminary data • Synoptic / synchronic maps/frames • Global MHD/non-MHD models • Disk data • (remapped in coordinates corrected in accordance with geometry & solar differential rotation) • Local “patch” maps • Local MHD/non-MHD models • AR • remapped

  4. Daily MHD model (steady-state) • Assumption: Polytrope in Eq. of state • Spatial resolution : ~ 5 degree • A few hours on 8-CPU(core) system. • With characteristics eq. matching fixed Br condition, the quasi-steady state be obtained • Outputs: • Open/closed coronal field structures • Rough estimation of flow speed and density • Magnetic field polarity at distant regions • Views from various directions • etc.

  5. Daily MHD model (steady-state) • Assumption: Polytrope in Eq. of state • Spatial resolution : ~ 5 degree • A few hours in 8CPUs system. • With characteristics eq. matching fixed Br condition, the quasi-steady state be obtained • Outputs: • Open/closed coronal field structures • Rough estimation of flow speed and density • Magnetic field polarity at distant regions • Views from various directions

  6. Daily MHD model (steady-state) • Assumption: Polytrope in Eq. of state • Spatial resolution : ~ 5 degree • A few hours in 8CPUs system. • With characteristics eq. matching fixed Br condition, the quasi-steady state be obtained • Outputs: • Open/closed coronal field structures • Rough estimation of flow speed and density • Magnetic field polarity at distant regions • Views from various directions

  7. Daily MHD model (steady-state) • Assumption: Polytrope in Eq. of state • Spatial resolution : ~ 5 degree • A few hours in 8CPUs system. • With characteristics eq. matching fixed Br condition, the quasi-steady state be obtained • Outputs: • Open/closed coronal field structures • Rough estimation of flow speed and density • Magnetic field polarity at distant regions • Views from various directions

  8. Daily MHD model (steady-state) • Assumption: Polytrope in Eq. of state • Spatial resolution : ~ 5 degree • A few hours on 8-CPU system. • With characteristics eq. matching fixed Br condition • The quasi-steady state be obtained • Outputs: • Open/closed coronal field structures • Rough estimation of flow speed and density • Magnetic field polarity at distant regions • Views from various directions • etc.

  9. Daily MHD model (with time-varying Br) • Assumption: Polytrope in Eq. of state • Spatial resolution : ~ 5 degree • A few hours on 8-CPU system. • With characteristics eq. matching time-varying Br • Under development • Outputs: time-evolutions of • Open/closed coronal field structures • Rough estimation of flow speed and density • Magnetic field polarity at distant regions • Views from various directions • etc.

  10. Surface magnetic field • From North pole, lon.90 dgr., south pole

  11. movie

  12. Models : contribution • surface flow: FLCT, ILCT, DAVE4VM, etc. • Complete or completed by induction Eq. • ier=(int)flct(argc,argv,deltat,deltas,sigma,nnx,nny,f1,f2,ef,ef,vx,vy,evx,evy,vm); • for quick-look purpose and/or • with calibrated data. • PSI’s MHD contribution ∂t Br=rot (v B)|r

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