State of NOAA-SEC/CIRES STEREO Heliospheric Models STEREO SWG Meeting, NOAA/SEC, Boulder, CO, March 22, 2004 Dusan Odstrcil University of Colorado/CIRES.

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Presentation transcript:

State of NOAA-SEC/CIRES STEREO Heliospheric Models STEREO SWG Meeting, NOAA/SEC, Boulder, CO, March 22, 2004 Dusan Odstrcil University of Colorado/CIRES & NOAA/Space Environment Center

Collaborators  Nick Arge – AFRL, Hanscom, MA  Chris Hood – University of Colorado, Boulder, CO  Jon Linker – SAIC, San Diego, CA  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 Supported by AFOSR/MURI and NSF/CISM projects

Input Data Analytic Models: - structured solar wind (bi-modal, tilted) - over-pressured plasma cloud (3-D) - magnetic flux-rope (3-D in progress) Empirical Models: - WSA source surface - SAIC source surface - CME cone model (location, diameter, and speed) Numerical Models: - SAIC coronal model (ambient + transient outflow)

Analytic Model – Distortion of ICME Study

Empirical model - Ambient Solar Wind

Numerical Model -- Magnetic Flux Rope Model Interface Compressed Plasma Shock Magnetic Leg Ejected Plasma

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 ]

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

Boundary Conditions Ambient Solar Wind + Plasma Cloud

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

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

Synthetic White-Light Imaging

Appearance of Transient Density Structure IPS observations detect interplanetary transients that sometime show two enhanced spots instead of a halo ring [Tokumaru et al., 2003] MHD simulation shows a dynamic interaction between the ICME and ambient solar wind that: (1) forms an arc-like density structure; and (2) results in two brighter spots in synthetic images

Evolution of Parameters at Earth

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

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 ]

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)

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 ]

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)

Evolution of Parameters at Earth

Remote Access IDL procedures ENLIL – Fortran/MPI/NetCDF Coronal Data (on MSS) Input Data (on PTMP) Output Data (on PTMP) ENKI -- web web Archive Data (on MSS) A/A – Java/VTK CDP ViServer ClientServer ENKI

ENKI – Interface to ENLIL

Remote Visualization: ENKI--IDL Preview of data before downloading processing and visualization, archiving, etc. Plot 1-D profiles and 2-D contours or surfaces of 1-D, 2-D, or 3-D data

Interplanetary Disturbances