1 / 160

Global MHD Simulation with BATSRUS from CCMC

Global MHD Simulation with BATSRUS from CCMC. ESS 265 UCLA1 (Yasong Ge, Megan Cartwright, Jared Leisner, and Xianzhe Jia). Outline. Description of Model Global Magnetophere Dayside Magnetopause and Solar Wind Cusp Region Investigation Magnetotail Investigation. BATS-R-US Model.

mab
Download Presentation

Global MHD Simulation with BATSRUS from CCMC

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 Simulation with BATSRUS from CCMC ESS 265 UCLA1 (Yasong Ge, Megan Cartwright, Jared Leisner, and Xianzhe Jia)

  2. Outline • Description of Model • Global Magnetophere • Dayside Magnetopause and Solar Wind • Cusp Region Investigation • Magnetotail Investigation

  3. BATS-R-US Model • BATS-R-US, the Block-Adaptive-Tree-Solarwind-Roe-Upwind-Scheme, was developed by the Computational Magnetohydrodynamics (MHD) Group at the University of Michigan, now Center for Space Environment Modeling (CSEM). It was designed using the Message Passing Interface (MPI) and the Fortran90 standard and executes on a massively parallel computer system. • The BATS-R-US code solves 3D MHD equations in finite volume form using numerical methods related to Roe's Approximate Riemann Solver. BATSRUS uses an adaptive grid composed of rectangular blocks arranged in varying degrees of spatial refinement levels. The magnetospheric MHD part is attached to an ionospheric potential solver that provides electric potentials and conductances in the ionosphere from magnetospheric field-aligned currents.

  4. Input parameters and boundary conditions • Fixed Solar Wind velocity of 400km/s, solar wind density of 5X106 protons/m3 and temperature of 1X105. • Two hours initialization with steady southward IMF. • Turning IMF northward for the last two hours. • Default ionosphere without corotation.

  5. Magnetic field lines t=00:00

  6. Magnetic field lines t=01:00

  7. Magnetic field lines t=01:58

  8. Magnetic field lines t=02:00

  9. Magnetic field lines t=02:04

  10. Magnetic field lines t=02:06

  11. Magnetic field lines t=02:08

  12. Magnetic field lines t=02:16

  13. Magnetic field lines t=02:30

  14. Magnetic field lines t=02:46

  15. Magnetic field lines t=03:00

  16. Magnetic field lines t=03:16

  17. Magnetic field lines t=03:20

  18. Magnetic field lines t=03:30

  19. Magnetic field lines t=03:46

  20. Magnetic field lines t=04:00

  21. Pressure + Velocity vectors t= 00:00 Noon-Midnight meridian view Equatorial view

  22. Pressure + Velocity vectors t= 01:00 Noon-Midnight meridian view Equatorial view

  23. Pressure + Velocity vectors t= 01:58 Noon-Midnight meridian view Equatorial view

  24. Pressure + Velocity vectors t= 02:00 Noon-Midnight meridian view Equatorial view

  25. Pressure + Velocity vectors t= 02:04 Noon-Midnight meridian view Equatorial view

  26. Pressure + Velocity vectors t= 02:06 Noon-Midnight meridian view Equatorial view

  27. Pressure + Velocity vectors t= 02:08 Noon-Midnight meridian view Equatorial view

  28. Pressure + Velocity vectors t= 02:16 Noon-Midnight meridian view Equatorial view

  29. Pressure + Velocity vectors t= 02:30 Noon-Midnight meridian view Equatorial view

  30. Pressure + Velocity vectors t= 02:46 Noon-Midnight meridian view Equatorial view

  31. Pressure + Velocity vectors t= 03:00 Noon-Midnight meridian view Equatorial view

  32. Pressure + Velocity vectors t= 03:16 Noon-Midnight meridian view Equatorial view

  33. Pressure + Velocity vectors t= 03:20 Noon-Midnight meridian view Equatorial view

  34. Pressure + Velocity vectors t= 03:30 Noon-Midnight meridian view Equatorial view

  35. Pressure + Velocity vectors t= 03:46 Noon-Midnight meridian view Equatorial view

  36. Pressure + Velocity vectors t= 04:00 Noon-Midnight meridian view Equatorial view

  37. Plasma temperature t= 00:00

  38. Plasma temperature t= 01:00

  39. Plasma temperature t= 01:58

  40. Plasma temperature t= 02:00

  41. Plasma temperature t= 02:04

  42. Plasma temperature t= 02:06

  43. Plasma temperature t= 02:08

  44. Plasma temperature t= 02:16

  45. Plasma temperature t= 02:30

  46. Plasma temperature t= 02:46

  47. Plasma temperature t= 03:00

  48. Plasma temperature t= 03:16

  49. Plasma temperature t= 03:20

  50. Plasma temperature t= 03:30

More Related