Sven Wedemeyer-Böhm, Eamon Scullion, Oskar Steiner, Luc Rouppe van der Voort, Jaime de la Cruz Rodriguez, Viktor Fedun and Robert Erdélyi Nature 486, 505–508 (28 June 2012) doi:10.1038/nature11202
Time progression of simulated solar thermal starting plumes. Rast, M. P., Mendoza, J., and Clyne, J. Compressible Thermal Starting Plume, Journal of Visualization, Vol. 10, No 3, July 2007
Toroidal magnetic fields generated by dynamo action in the convection zone of a star like our sun, but rotating more rapidly at three times the
current solar rate, as our own sun did when younger. Ben Brown, University of Colorado
Simulation of a Galactic globular cluster orbiting our galaxy as the of intra-cluster medium gas is stripped from the GC's gravitational potential
due to the ram-pressure of the hot, low density Galactic halo medium. William Priestley, Liverpool John Moores University.
Magnetic energy and magnetic field lines from the average in time velocity dynamo mode with Taylor-Green forcing. Imagery courtesy of Yannick Ponty, Observatoire de la Cote d,Azur
Visualization of magnetic field lines in a magnetic flux tube. Field lines seeded using data probe inserted in flux tube. Magnetic field results from simulation of the buoyant rise of a twisted magnetic flux tube through the solar connective envelope towards the solar surface. Data courtesy of Yuhong Fan, NCAR
Side-by-side comparison of vorticity and vertical momentum in solar flow simulation. Flow seeds injected at maximal vorticity using data probe. Color indicates elapsed time of particle in flow. Data courtesy of Mark Rast (NCAR and Univ. of Colorado)
Visualization of unsteady flow in a momentum field based on simulation of the interior of the Sun. Arrows indicate motion during one time
step. Data courtesy of Mark Rast (NCAR and Univ. of Colorado).
