MHD model in HMI pipeline

MHD model in HMI pipeline

HMI/AIA science team meetingSep. 8 -- 11, 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, (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

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.

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

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

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

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.

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.

• 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,vx,vy,evx,evy,vm);

– for quick-look purpose and/or – with calibrated data.

• PSI’s MHD contribution

∂t Br=rot (v B)|r