High Resolution 2-D Numerical Simulation of Emergence of Magnetic Flux Through the Solar Atmosphere

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)."