1 / 26

Global MHD Simulations of Dayside Magnetopause Dynamics. THEMIS Event: May 20, 2008 20:30 – 22:30

Global MHD Simulations of Dayside Magnetopause Dynamics. THEMIS Event: May 20, 2008 20:30 – 22:30. M. M. Kuznetsova, D. G. Sibeck , M. Hesse , L. Rastaetter , T. Gombosi. http:// ccmc.gsfc.nasa.gov. NASA Goddard Space Flight Center. Global MHD Simulation Model.

mimi
Download Presentation

Global MHD Simulations of Dayside Magnetopause Dynamics. THEMIS Event: May 20, 2008 20:30 – 22:30

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. Global MHD Simulations of Dayside Magnetopause Dynamics. THEMIS Event: May 20, 2008 20:30 – 22:30 M. M. Kuznetsova, D. G. Sibeck, M. Hesse, L. Rastaetter, T. Gombosi http://ccmc.gsfc.nasa.gov NASA Goddard Space Flight Center

  2. Global MHD Simulation Model BATS-R-US (CSEM, University of Michigan)uses an adaptive grid composed of rectangular blocks arranged in varying degrees of spatial refinement levels. Resolution at Dayside Magnetopause Including Flanks: 1/16 Re 15 – 20 mln grid cells

  3. Runs with Modeled Conditions Kuznetsova et al, 2004 Solar Wind Parameters: N = 2 cm –3 , T = 20,000 Ko, Vx = 300 km/s, |B| = 5 nT IMF Turning From Northward Orientation (θ= 0) to IMF Clock angleθ < 120o:

  4. Sub-Solar FTE Structure Theta = 120o BATSRUS Cluster Pressure Masha_Kuznetsova_031704_4a Pressure

  5. Vortices Generation at the Flanks Close to regions of large flow velocity shear and almost anti-parallel magnetic field. Theta = 120o

  6. Vortices at the Flanks for Southward IMF Theta = 180o Joe_Borovsky_040207_1c

  7. THEMIS Dayside Event: May 20, 2008, 20:30 – 22:30 Solar wind propagated from ACE to 33 Re Global Magnetosphere at 22:00 Resolution at Dayside Magnetopause: 1/16 Re

  8. Weak Magnetic Field Cavity Follows the FTE. Time: 20:51:10 UT Magnetic field (|B|) Pressure (P) Density (N) Velocity (|V|)

  9. Significant Deviations from 2D Tilted Flux Tube Z = - 1.5 Re Slice - 1 Re - 2 Re + 1 Re

  10. Start Points for Field Line Tracing at Z = -1.5 Re Slice .

  11. View from the South

  12. View from the Sun Start points for field line tracing at Z = - 1.5 Re slice

  13. Component Reconnection Near Sub-Solar Region (Y ~ 0 – 2 Re) And Anti-Parallel Reconnection at Flanks (Y ~ 12 - 15 Re)

  14. FTE at Flanks (Y = 12 Re) is Connected to FTE at the Sub-Solar Region ( Y = 0 ). X-slice Y-slice Z-slice

  15. Slices Through FTE Magnetic Field Strength X = 1 |Y – 15| < 2 Y = 0 Z = - 1.5 |Y - 12| < 2 Time: 20:51:10 UT

  16. Slice Through FTE: Y = 0 Time interval: 20:40 – 21:00 Magnetic Field Strength

  17. FTE Bulge with Strong Core Field Time: 20:51:10 UT Pressure (P) Magnetic field (|B|) The plasma pressure exhibit a ring-shaped structure surrounding a central depression Density (N) Velocity (|V|) The flow around the flux rope is largest at the magnetosphere side.

  18. Signature of Bended Flux Rope (FTE) Near Sub-Solar Region Y = 0 Y = - 2 Re Y = 2 Re + 2 Re + 2 Re Bended Flux Rope (FTE) Near Sub-Solar Region

  19. Signature of Bended Flux Rope (FTE)

  20. Signature of Bended Flux Rope

  21. Slice Through FTE: X = 1 |Y - 15| < 2 Time interval: 20:40 – 21:00 Magnetic Field Strength

  22. Supplementary Slides

  23. Click Here

More Related