MHD model in HMI pipeline HMI/AIA science team meeting Sep , 2009 Stanford, CA HMI/AIA science team meeting Sep , 2009 Stanford, CA

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 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

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 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

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. 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.

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 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

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 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

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 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

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. 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.

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. 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.

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

movie

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,v x,vy,evx,evy,vm); –for quick-look purpose and/or –with calibrated data. PSI’s MHD 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,v x,vy,evx,evy,vm); –for quick-look purpose and/or –with calibrated data. PSI’s MHD contribution ∂ t B r =rot (v  B) | r