1 / 25

3-D Solar Wind and Interplanetary Disturbance Modeling

This study presents a comprehensive analysis of solar wind and interplanetary disturbances using analytic, empirical, and numerical models. It explores the evolution of density structures and the appearance of transient density structures in synthetic white-light imaging. The interaction between the disturbances and the ambient solar wind is also examined. The study provides important insights into the propagation and behavior of interplanetary shocks and coronal mass ejections.

cnordberg
Télécharger la présentation

3-D Solar Wind and Interplanetary Disturbance Modeling

An Image/Link below is provided (as is) to download presentation Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author. Content is provided to you AS IS for your information and personal use only. Download presentation by click this link. While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server. During download, if you can't get a presentation, the file might be deleted by the publisher.

E N D

Presentation Transcript

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

  2. 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 Collaborators Supported by AFOSR/MURI and NSF/CISM projects

  3. 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)

  4. Analytic Model – Distortion of ICME Study

  5. Empirical model - Ambient Solar Wind

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

  7. Ambient Solar Wind Models CU/CIRES-NOAA/SEC 3-D solar wind model based on potential and current-sheet source surface empirical models SAIC 3-D MHD steady state coronal model based on photospheric field maps [ SAIC maps – Pete Riley ] [ WSA maps – Nick Arge ]

  8. CME Cone Model 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 [ Zhao et al., 2001 ]

  9. Boundary Conditions Ambient Solar Wind + Plasma Cloud Ambient Solar Wind

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

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

  12. Synthetic White-Light Imaging

  13. 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

  14. Evolution of Parameters at Earth

  15. May 12, 1997 – Interplanetary Shock 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 • Shock propagates in a fast stream and • merges with its leading edge 1.0 AU

  16. Case A1 Case A3 [ SAIC maps -- Pete Riley ] Fast-Stream Position Ambient state before the CME launch Disturbed state during the CME launch Ambient state after the CME launch

  17. [ SAIC maps -- Pete Riley ] Effect of Fast-Stream Position Case A1 Case A3 Earth : Interaction region followed by shock and CME (not observed) Earth : Shock and CME (observed but 3-day shift is too large)

  18. Case A2 Case B2 [ SAIC maps -- Pete Riley ] Fast-Stream Evolution Ambient state before the CME launch Disturbed state during the CME launch Ambient state after the CME launch

  19. [ SAIC maps -- Pete Riley ] Effect of Fast-Stream Evolution Case A2 Case B2 Earth : Interaction region followed by shock and CME (not observed) Earth : Shock and CME (observed but shock front is radial)

  20. Evolution of Parameters at Earth

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

  22. ENKI – Interface to ENLIL

  23. ENKI – Interface to ENLIL

  24. 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

  25. Interplanetary Disturbances

More Related