Heliospheric MHD Modeling of the May 12, 1997 Event MURI Meeting, UCB/SSL, Berkeley, CA, March 1-3,...
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Transcript of Heliospheric MHD Modeling of the May 12, 1997 Event MURI Meeting, UCB/SSL, Berkeley, CA, March 1-3,...
![Page 1: Heliospheric MHD Modeling of the May 12, 1997 Event MURI Meeting, UCB/SSL, Berkeley, CA, March 1-3, 2004 Dusan Odstrcil University of Colorado/CIRES &](https://reader036.fdocuments.us/reader036/viewer/2022062421/56649d405503460f94a19c5d/html5/thumbnails/1.jpg)
Heliospheric MHD Modeling of the May 12, 1997 Event
MURI Meeting, UCB/SSL, Berkeley, CA, March 1-3, 2004
Dusan Odstrcil
University of Colorado/CIRES & NOAA/Space Environment Center
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Collaborators
Nick Arge – AFRL, Hanscom, MA
Chris Hood – University of Colorado, Boulder, CO
Rob Markel – University of Colorado, Boulder, CO
Leslie Mayer – University of Colorado, Boulder, CO
Vic Pizzo – NOAA/SEC, Boulder, CO
Pete Riley – SAIC, San Diego, CA
Marek Vandas – Astronomical Institute, Prague, Czech Republic
Xuepu Zhao – Stanford University, Standford, CA
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Ambient Solar Wind Models
SAIC 3-D MHD steady state coronal model based on photospheric field maps
CU/CIRES-NOAA/SEC 3-D solar wind model based on potential
and current-sheet source surface empirical models
[ SAIC maps – Pete Riley ] [ WSA maps – Nick Arge ]
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CME Cone Model
[ Zhao et al., 2001 ]
Best fitting for May 12, 1997 halo CME
• latitude: N3.0• longitude: W1.0• angular width: 50 deg
• velocity:650 km/s at 24 Rs
(14:15 UT)• acceleration: 18.5 m/s2
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Boundary Conditions
Ambient Solar WindAmbient Solar Wind
+ Plasma Cloud
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Latitudinal Distortion of ICME Shape
ICME propagates into bi-modal solar wind
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Evolution of Density Structure
ICME propagates into the enhanced density of a streamer belt flow
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Synthetic White-Light Imaging
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Interplanetary Disturbances
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Evolution of Parameters at Earth
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May 12, 1997 – Interplanetary Shock
• Shock propagates in a fast stream and
merges with its leading edge
Distribution of parameters in equatorial plane Evolution of velocity on Sun-Earth line
0.2 AU
0.4 AU
0.6 AU
0.8 AU
1.0 AU
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Fast-Stream Position
Ambient state before the CME launch
Disturbed state during the CME launch
Ambient state after the CME launch
Case A1 Case A3
[ SAIC maps -- Pete Riley ]
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Effect of Fast-Stream Position[ SAIC maps -- Pete Riley ]
Case A1 Case A3
Earth : Interaction region followed by shock and CME (not observed)
Earth : Shock and CME (observedbut 3-day shift is too large)
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Streamer-Belt Disruption?
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Fast-Stream Evolution
Ambient state before the CME launch
Disturbed state during the CME launch
Ambient state after the CME launch
Case A2 Case B2
[ SAIC maps -- Pete Riley ]
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Effect of Fast-Stream Evolution[ SAIC maps -- Pete Riley ]
Case A2 Case B2
Earth : Interaction region followed by shock and CME (not observed)
Earth : Shock and CME (observedbut shock front is radial)
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Fast-Stream Evolution
Ambient state before the CME launch
Disturbed state during the CME launch
Ambient state after the CME launch
Case A2 Case B2
[ WSA maps -- Nick Arge ]
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Effect of Fast-Stream Evolution[ WSA maps – Nick Arge ]
Case A2 Case B2
Earth : Interaction region followed by shock and CME (not observed)
Earth : Shock and CME (observedbut shock front is radial)
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Daily-Updated Synoptic Maps[ WSA maps – Nick Arge ]
Evolving velocity structure at 21.5 Rs due to changes in photospheric field
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Magnetic Flux Rope[ 3D force-free model – Marek Vandas ]
Toroidal structure emerges into computational domain