suntoionosphere modeling at the community coordinated ...ks/symposium/talks/lr_modeling_at_… ·...
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SuntoIonosphereModeling at the CommunityCoordinated Modeling Center
NASA Goddard Space Flight Center
Lutz Rastaetter
http://ccmc.gsfc.nasa.gov
11/1/06
Outline
• The CommunityCoordinated Modeling Center (CCMC)
• Models at CCMC– Real time simulations– Runs on Request
• Examples of Research at CCMC– Polar cap size and location– Fluxtransfer events
• Summary
The CommunityCoordinated Modeling Center
CCMC goal: Facilitate community use of space science modelsModeling context is critical for data analysis in space physics• Models at the CCMC can produce vastly more science results.•Models can be validated and be prepared for a wider range of uses (“space weather forecasting”)
CCMC is a multiagency partnership including NASA (National Aeronautic and Space Administration), NSF (National Science Foundation),
NOAA (National Oceanic and Atmospheric Administration),CCMC was started in 1999 by Michael Hesse, now has 12 staff members and offers
more than 20 models and products.
Models at CCMC
SWMF / SC,IH,GM,IM,IE,UA
Fok RCFok RB
MAS
PFSS
Helio. Tomog.
ENLIL
Exosph. SWBATSRUSOpenGGCM
SAMI2 CTIPWeimerIE solversWSA
USUGAIM
RunsOnRequest• Userdefined runs
• Interactive visualization
• Comparisons between Models and Observations
• Export of model outputs for users' own analyses
Runs on Request
Executed runs (Aug. 2006): Oct. 24, 2006Solar & Heliosphere : 128 223Global magnetosphere: 607 629Inner magnetosphere: 97 100Ionosphere: 166 172Total: 998 1124 runs
0
200
400
600
800
1000
2001 2002 2003 2004 2005 2006
Global Magnetosphere Inner Magnetosphere
Ionosphere/Thermosphere Solar and Heliosphere
On the Web:
http:/ccmc.gsfc.nasa.gov/
Request A Model Run
View Model Run Results
Runs on Request
• RealEvent simulations (Bastille Day, Halloween Storms,…)
• Modeled Events (arbitrary date, userdefined input data)
• Webbased visualization (examples follow in this presentation)– 1D satellite tracks
– 2D ionosphere ElectroDynamics
– 3D model data in various coordinate systems in the solar corona, heliosphere, Earth's magnetosphere and ionosphere/thermosphere.
• Model output data export– as text files
– CDF format with interpolation library for C/C++ and Fortan codes.
R<5: Model Magnetic fieldR<30: MHD solution
Models : Solar Corona
magnetogramdriven, steadystate solutions
magnetogram data + analyses
Real time run:solar wind at EarthHeliosphere Model
MHD solar wind model,with positions of inner planets
Models: Heliosphere
coronal models
Meridional tail section
Models: Earth's Magnetosphere
Solarwind driven (ACE, WIND)two global MHD models1D track, 2D plots and 3D field lines
Virtual satellite: cluster1
Slice and3D field lines
Models: Magnetosphere (real time)
Solar wind inputs
Magnetosphere
Ionospheric Electro.Dyn.
Models: Magnetosphere (real time)
BATSRUS (since 2002), • 0.5 RE resolution, 301536 cells
SWMF (2006): • 0.25 RE resolution, 755136 cells
• innermagnetosphere physics with RiceConvection Model: => better Region2 currents
17:40, Mon. Oct. 23, 2006
Runson Request grids:
Typically 23 million cells,
up to 12 million possible.
Synoptic maps:GAIM NmF2 (max. Ne in F2layer)
Models: IonosphereIonosphereThermosphere• Standalone, driven by solar wind,
solar radiation: CTIP, SAMI2• Dataassimilative:
USUGAIM/IFM
Vertical slice:CTIP Tn at constant longitude
Realtime run, every 5 minutes Weimer '05 Potential (PHI), Currents (FAC)
Models: Ionosphere (real time)
IonosphericElectrodynamics (IE)– Standalone model, driven by solar wind:
Weimer (2K, 2005 versions)
Solar wind Aurora observed by POLAR and IMAGE
Polar cap: region of open Bfield lines in model
vs.
poleward edge of
emissions in observ.
Research: Polar cap sizeBastille Day Storm, July 14, 2001, at Earth, July 15
Research: Polar cap size
Bastille Day (cont.):Models roughly follow observed changes in size but follow the solar wind Bz more closely than the observations.
Observed average magnetic colatitude of boundary varies between 5º (15:20 UT) and 28º (20:10 UT)Range from model results is smaller.
Research: Flux Rope FormationAnatomy of flux transfer event seen by ClusterSonnerup, Hasegawa, and Paschmann, Geophys. Res. Letters, L11803, 2004
P |B|
GradShafranov reconstruction of flux rope from Cluster dataat magnetopause:Pressure Pmagnetic field |B|Images turned to match subsolar region…
V V
Research: Flux Rope evolutionSimulation: solar wind clock angle: θ = 120
M. Kuznetsova, 2005 , run with 1/16 RE resolution at magnetopause
P [nPa] B [nT]
V [km/s]
B field lines
V [km/s]
Research: Mission support, collaborations
CLUSTER:A number of researchers used CCMC for magnetopause and cusp features.
CASSINI: CCMC offers runs covering outer heliosphere.
IRIDIUM:Study to compare modeled fieldaligned currents with observations is planned.
STEREO:CCMC keeps archive of daily solarheliospheric runs.Close collaboration expected during satellite operation.
THEMIS: 5satellite constellation to study substormsin magnetospheric tail (2007 launch)
X
Users employ simulation runs requested at CCMC
Summary
• CCMC is a valuable asset in space physics.
• Models are free to use by anyone for research.
• Modeling becomes more important to analyze
complex observations.
CCMC web site: ccmc.gsfc.nasa.gov