CISM

SOHO image animation (57k)
images from SOHO-EIT

SolarCISM Gallery

Movie of a 2D simulation of a flux rope CME using CISM models


Click on the above image to view an animation of a two-dimensional simulation of a flux-rope CME, generated in the SAIC coronal model by helmet streamer shearing and photospheric flux cancellation, propagating into the ENLIL solar wind model. Animation: D. Odstrcil


Movie from a 3D simulation of an erupted flux rope CME using CISM coupled coronal and solar wind models


Click on the above image to view an animation of a 3-dimensional simulation of interplanetary fields disturbed by a flux-rope CME. The CME was generated in the SAIC coronal model by helmet streamer shearing and photospheric flux cancellation, and propagated into the ENLIL solar wind model. Animation: D. Odstrcil


Movie of the interplanetary shock from the 3D simulation of an erupted flux rope CME shown above.


Click on the above image to view an animation of the interplanetary shock front generated by the 3-dimensional flux-rope CME illustrated above. Animation: D. Odstrcil


Simulation of a magnetic flux tube emerging into a preexisting potential bipolar field

Top View

Side View

Click on the images to see animated simulations of a flux tube emerging into a preexisting bipolar field. These animations (top view and side view) show how a magnetic flux tube (white lines) initially located below the surface emerging into the solar atmosphere where a bipolar potential field (red lines) exists. After emergence the field lines expand rapidly, which strongly push out the overlying bioplar field lines. A color map at z = 0 shows the vertical magnetic flux at the surface. The units of length, time, velocity, and magnetic field are 540 km, 50 s, 11 km/s, and 570 G, respectively. Animation: T. Magara


Simulation of a magnetic flux tube emerging into a field-free corona

Side View

Click on the images to see animated simulations of a flux tube emerging into a preexisting coronal field arcade. This animation shows the evolution of a twisted flux tube emerging from below the photosphere into a field-free corona. The gray and black field lines represent the outer and inner (initially corresponds with the axis) field line of the flux tube. The horizontal map shows the photosphere. Animation: T. Magara


3D simulation of a propagating dynamic pressure in the ENIL solar wind model, with stream structure for the May 12, 1997 halo CME event



Click on this image to view a movie from a 3D simulation of a propagating dynamic pressure pulse with circular cross section in the ENLIL solar wind model. The background solar wind stream structure and pressure pulse characteristics have been chosen to represent the May 12, 1997 halo CME event under study. The solar wind boundary conditions are based on the SAIC coronal model magnetic fields. Animation: D. Odstrcil