mhd model in hmi pipeline
DESCRIPTION
HMI/AIA science team meeting Sep. 8 -- 11, 2009 Stanford, CA. MHD model in HMI pipeline. MHD models. Input : as initial & boundary values, the magnetic field data, in various formats and cadences, (and plasma parameters from observations) - PowerPoint PPT PresentationTRANSCRIPT
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