Comparing volume renderings of two different scalar fields

Wintertime Polar Vortex. Data courtesy of Mark Taylor, Los Alamos National Lab.

Magnetic fields on the solar surface. Data courtesy of Yuhong Fan, High Altitude Observatory, National Center for Atmospheric Research

Fine scale turbulence. Data courtesty of Pablo Mininni, Institute for Mathematics Applied to Geosciences, National Center for Atmospheric Research

Visualization of hydrodynamic turbulent flow around a vortex tube.  Flow seeded by rake shown in scene. Data courtesty of Pablo Mininni, Institute for Mathematics Applied to Geosciences, National Center for Atmospheric Research

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).

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  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

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

2D+time turbulent mixing in a cylinder. Data courtesy of Benjamin Kodach, Universite de Provence

Magnetic field lines from stellar convection simulations on a sphere. Image courtesy of Ben Brown, University of Colorado.

Direct numerical simulation of salt sheets and turbulence in a double-diffusive shear layer. Satoshi Kimura and William Smyth, University of Oregon

Air convection in the atmosphere over a heated plane. Z. Piotrowski, P. Smolarkiewicz, S Malinoski, and A. Wyszogradzki, University of Warsaw and NCAR

Formation of vorticity "smoke rings" under the action of Crow instability in a simulation of the soloar interior. G. Vasil, University of Colorado

Simulated star formations with RAMSES. Paolo Padoan, UCSD.

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.

Subcritical Dynamo Bifurcation in the Taylor-Green Flow. Y. Ponty, et al., Observatoire de la Cote d'Azur, Nice

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

Downward flowing thermal starting plume. Mark Rast, University of Colorado.

Simulation of oceanic mesoscale eddy turbulence showing baroclinic instability of a large-scale zonal jet that produces many mesoscale eddies that strongly interact, resulting in filaments that spawn vortices.

Patrice Klein , Sylvie Le Gentil and Bach Lien Hua, scientists at the Laboratoire de Physique des Oceans, IFREMER.

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

WRF simulation of frost event over Georgia in April. Flow of particles released in the mountains north of Atlanta. Thara Prabhakaran, University of Georgia

WRF simulation of frost event over Georgia in April. Thara Prabhakaran, University of Georgia