High Resolution 2-D Numerical Simulation of Emergence of Magnetic Flux Through the Solar Atmosphere
This series of animations (animations 107, 1416, 1417, and 1418) show sheets of magnetic flux undergoing velocity perturbations. The conditions for each simulation are outlined within the video.
Density and magnetic flux surfaces from a simulation of magnetic flux in the solar atmosphere undergoing velocity perturbations. This run has a vertical scale height of 6.8 million meters.
Video slate image reads "High Resolution Two Dimensional Numerical Simulation of Emergence of Magnetic Flux Through the Solar Atmosphere
M.L. Rilee(NRC/GSFC)
D. Spicer(GSFC) and R. Sudan(Cornell Univ.)
June 1996".
Descriptive image reads, "Ideal MHD in a model photosphere/corona:
Structured spatial mesh: resolution (nx, ny) = (300, 500)
Flux-Corrected-Transport, 4th order spatial differences.
Predictor-Corrector time advance.
Periodic in x, hard wall at bottom.
Characteristic outflow-no inflow at top.
Initial condition:
A sheet of magnetic flux suffers a velocity perturbation;
the ratio of specific heasts is 1.05,
(ct. Shibata et al., 1989 APJ 345 584)."
Credits
Please give credit for this item to:
NASA/Goddard Space Flight Center
Scientific Visualization Studio
-
Animator
- Liam Krauss (Hughes STX)
-
Scientists
- Dan Spicer (NASA/GSFC)
- M. L. Rilee (NASA/GSFC)
- R. Sudan (Cornell University)
Release date
This page was originally published on Tuesday, May 21, 1996.
This page was last updated on Wednesday, May 3, 2023 at 2:00 PM EDT.