General Gallery
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
Visualization of Cryo-EM Tomographic reconstructions of frozen-hydrated Deinococus Radiodurans, prepared by plunge-freezing into liquid ethene and later transfered to liquid nitrogen. Imagery courtesty of Cristina Siegerist (LLNL).
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
New Journal of Physics, 10th Anniversary Highlights (first row, 2nd column, and 2nd row, 3rd column).
Passage of a cold front on 18th February 2008 over Georgia. The convergence of moisture ( colored flow lines with red corresponding to high moisture content and green color with low moisture content) along the front is presented using three dimensional vorticity. Thara Prabhakaran, University of Georgia
Flapping magnetic field lines. Aake Nordlund, Niels Bohr Institute.
Vortices in the eye wall of a WRF hurricane simulation, illustrated by a combined streamline and image-based flow visualization. Yongsheng Chen, MMM/NCAR
Simulation of bacteria in a turbulent flow. A spherical patch of nutrient (shown by the green isosurface) was released at an earlier time in fully-developed isotropic turbulence. High concentrations of bacteria are shown in blue. The bacteria have the ability to swim up nutrient gradients (known as chemotaxis) and start uniformly distributed throughout the volume, but are able to cluster around the nutrient filaments. John Taylor, MIT
Small scale vorticity in fully developed turbulence. Michael Wilczek, Institute for Theoretical Physics, University of Muenster.
Temperature fluctuations in compositionally driven double diffusive convection. Stephan Stellmach, UCSC
A snapshot in time of a numerically simulated supercell thunderstorm including reflectivity, surface cold pool, and selected streamlines. Leigh Orf, Central Michigan University