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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 &

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Presentation on theme: "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 &"— Presentation transcript:

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 & NOAA/Space Environment Center

2 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

3 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 ]

4 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 R s (14:15 UT) acceleration: 18.5 m/s 2

5 Boundary Conditions Ambient Solar Wind + Plasma Cloud

6 Latitudinal Distortion of ICME Shape ICME propagates into bi-modal solar wind

7 Evolution of Density Structure ICME propagates into the enhanced density of a streamer belt flow

8 Synthetic White-Light Imaging

9 Interplanetary Disturbances

10 Evolution of Parameters at Earth

11 May 12, 1997 – Interplanetary Shock Shock propagates in a fast stream and merges with its leading edge Distribution of parameters in equatorial planeEvolution of velocity on Sun-Earth line 0.2 AU 0.4 AU 0.6 AU 0.8 AU 1.0 AU

12 Fast-Stream Position Ambient state before the CME launch Disturbed state during the CME launch Ambient state after the CME launch Case A1Case A3 [ SAIC maps -- Pete Riley ]

13 Effect of Fast-Stream Position [ SAIC maps -- Pete Riley ] Case A1Case A3 Earth : Interaction region followed by shock and CME (not observed) Earth : Shock and CME (observed but 3-day shift is too large)

14 Streamer-Belt Disruption?

15 Fast-Stream Evolution Ambient state before the CME launch Disturbed state during the CME launch Ambient state after the CME launch Case A2Case B2 [ SAIC maps -- Pete Riley ]

16 Effect of Fast-Stream Evolution [ SAIC maps -- Pete Riley ] Case A2Case B2 Earth : Interaction region followed by shock and CME (not observed) Earth : Shock and CME (observed but shock front is radial)

17 Fast-Stream Evolution Ambient state before the CME launch Disturbed state during the CME launch Ambient state after the CME launch Case A2Case B2 [ WSA maps -- Nick Arge ]

18 Effect of Fast-Stream Evolution [ WSA maps – Nick Arge ] Case A2Case B2 Earth : Interaction region followed by shock and CME (not observed) Earth : Shock and CME (observed but shock front is radial)

19 Daily-Updated Synoptic Maps [ WSA maps – Nick Arge ] Evolving velocity structure at 21.5 Rs due to changes in photospheric field

20 Magnetic Flux Rope [ 3D force-free model – Marek Vandas ] Toroidal structure emerges into computational domain

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