Movies
Numerical solutions of quantal four-body breakup
Movie (12 MB MPEG)
Description:
The movie shows the time evolution of a wavepacket scattering from the Helium atom. The three coordinates represent the radial positions of each electron.
Scientific Calculations: Mitch Pindzola, Auburn University
Visualization:
Cristina Siegerist, Lawrence Berkeley National Laboratory
Scientific References:
Triple photoionization of the Lithium atom,
J. Colgan, M.S. Pindzola, and F. Robicheaux, Physical
Review Letters, 93, 053201 (2004);
Double photoionization of the Hydrogen molecule
J. Colgan, M.S. Pindzola, and F. Robicheaux,
Journal of Physics B Letters, submitted;
Electron impact double ionization of the Helium atom
M.S. Pindzola, F. Robicheaux. J. Colgan, M.C. Witthoeft,
J.A. Ludlow, Physical Review A 70, 032705 (2004).
Vortex dynamics and mixing in a transverse jet
Movie 1 (69 MB Quicktime)
Movie 2 (62 MB Quicktime)
Description:
The movies show two different perspectives of a starting
jet in a cross flow stream, the type used in fuel injection, dilution
and cooling, drug delivery, etc., visualized using vorticity
contours, and depicting how large magnitudes migrate from large
scales to smaller scales downstream.
Scientific Calculations:
Youssef Marzouk, Daehyun Wee and Ahmed Ghoniem; Massachusetts Institute of Technology
Visualization:
Youssef Marzouk and Daehyun Wee, MIT
Magnetohydrodynamic Simulation of the Sustained Spheromak Physics Experiment
Movie (2.2 MB MPEG)
Description:
This animation shows results from a 3D nonlinear magnetohydrodynamics
(MHD) simulation of the 46xx series of plasma discharges in the SSPX
experiment at Lawrence Livermore National Laboratory [H. S. McLean et al.,
Phys. Rev. Lett. 88, 125004-1 (2002)]. The physical region is cylindrical,
and the graphics illustrate a radial-axial cross-section. The evolving
color contour plot to the left of the cylindrical axis shows the azimuthal
average of the electrical current density that is parallel to the magnetic
field. The color contour plot on the right shows plasma temperature,
overlaid with contours of the azimuthally averaged poloidal magnetic flux
function. The curved surfaces represent solid metal electrodes, and an
applied potential difference drives electrical current through the plasma.
The discharge first sweeps plasma and the initial poloidal flux distribution
into the large part of the chamber. As the electrical current column pinches
through Lorentz forces, it becomes unstable to a helical MHD kink mode, which
reconnects magnetic field-lines and converts toroidal magnetic flux into
additional poloidal magnetic flux. By reducing the injector current after
the formation phase, the confinement properties of the magnetic field
distribution improve, and the peak plasma temperature increases. The numerical calculations have been performed with the NIMROD code (http://nimrodteam.org and
C. R. Sovinec et al., J. Comput. Phys. 195, 355 (2004)).
Scientific Calculations:
C. R. Sovinec, University of Wisconsin-Madison, and B. I. Cohen, Lawrence Livermore National Laboratory
Visualization:
C. R. Sovinec, University of Wisconsin-Madison
References:
C. R. Sovinec et al., "Numerical Investigation of Transients in the SSPX Spheromak," submitted for publication in Physical Review Letters (see http://www.cptc.wisc.edu/sovinec_research);
B. I. Cohen et al., "Spheromak Evolution and Energy Confinement," in preparation for publication in Physics of Plasmas.
X-Band Linear Collider R&D
Description:
Dark current simulation in an X-Band 30-cell Constant Gradient Accelerating
Structure. At high accelerating gradients, high surface fields lead to
field emission (in red) which produces secondary emission (in green)
upon impact with the wall. The emitted electrons that are captured by
the accelerating fields, form the dark current that can
discrupt the main beam and interfere with the detector operation
down stream at the interaction point. Parallel particle tracking
code, Track3P, provides estimates of the dark current
pulse generated that compares well with measured data.
Visualization:
Greg Schussman, Stanford Linear Accelerator Center
Description:
Wakfield Analysis of the X-Band 55-cell Damped, Detuned Accelerating Structure. Parallel time domain solver Tau3P simulates the electromagnetic fields excited by a beam transiting an actual prototype and calculates the wakefields seen by a trailing witness beam. Numerical results verify the wakefield suppression scheme by damping and detuning, and they are in good agreement with results from frequency domain computations using the parallel eigenmode solver Omega3P.
Scientific Calculations:
Nate Folwell, Lixin Ge, Adam Guetz, Valentin Ivanov, Marc Kowalski, Liequan Lee, Zenghai Li, Cho Ng, Greg Schussman, Ravi Uplenchwar, Liling Xiao, and Kwok Ko; Stanford Linear Accelerator Center.
Could There be a Hole in Type Ia Supernovae?
Description:
The video shows an illustration of the Monte Carlo method for performaing
spectopolametric synthesis calculations for a Type Ia supernova. The
points coming out are individual photons (color-coded by wavelength) which
scatter multiple times randomly as they make their way out of the
atmosphere. Here the supernova has exploded near its companion
and has had a hole carved out of it.
Description:
The spectra and polarization as a function of viewing angle for the
supernova scenario described above. The spectrum is hot and blue
looking down the hole (where the photons can easily escape from the lower
hotter regions of the SN) and cooler as the angle moves to the side and we
can only see the outer layers. The polarization is strongest when the
geometry is the least symmetrical, looking down the side of the hole.
Scientific Calculations:
Daniel Kasen, Peter Nugent, R.C. Thomas, and Lifan Wang; Lawrence Berkeley National Laboratory
Visualization:
NERSC visualization group and Cristina
Siegerist, Lawrence Berkeley National Laboratory
High-Quality Electron Beams from a Laser Wakefield Accelerator Using
Plasma-Channel Guiding
Movie 1 (1.8 MB Quicktime)
See Laser Wakefield Acceleration: Channeling the Best Beams Ever.
Description:
The wake density perturbation driven by the laser (top
frame) and the resulting electron bunch accelerated (bottom frame).
Movie 2 (2.3 MB Quicktime)
Description:
An alternate view, including the
laser pulse envelope and the accelerating (Ex) field
of the wake as well as the electron phase space (x-ux).
Scientific Credits:
Cameron Geddes, LBNL/UC Berkeley; Csaba Toth, LBNL;
Jeroen van Tilborg, LBNL/Technische Universiteit Eindhoven;
Eric Esarey, LBNL; Carl Schroeder, LBNL;
David Bruhwiler, Tech-X; Chet Nieter, Tech-X; John Cary,
Tech-X/U Colorado; and Wim Leemans, LBNL.
Rayleigh-Taylor Unstable Flames in a Type Ia Supernova
Description:
A visualization of the carbon fuel in a three-dimensional direct numerical
simulation of the reactive Rayleigh-Taylor instability in a type Ia
supernovae.
These supernovae are powered by the thermonuclear energy release from a
burning front that propagates outward from the center of a white dwarf
star. This burning front accelerates through the increase in surface area
driven by hydrodynamic instabilities (chiefly, the Rayleigh-Taylor
instablity). This simulation is the first three-dimensional, resolved
calculation of a Rayleigh-Taylor unstable flame. Here, only a small
portion of the star is followed -- about 1/2 meter on a side. As the
instability evolves, we see the flame transition from a smooth laminar
flow, into the nonlinear Rayleigh-Taylor regime, and finally go fully
turbulent. This calculation was performed on the seaborg machine at
NERSC, on 512-processors.
Description:
This animation shows a small region from that shown in the previous movie.
Visualization: Marc Day, Lawrence Berkeley National Laboratory
Description:
Two dimensional direct numerical simulations of reactive Rayleigh-Taylor
instabilities in Type Ia supernovae. Here we show the evolution of a
carbon thermonuclear flame, propagating upward, in the presence of a
strong gravitational field. The hot ash behind the flame buoyantly rise,
wrinking the flame and accelerating, while the reactions consume the
fingers of heavier fuel that fall downward. Several fields are shown.
This calculation is at a density of 1.5x107 g/cc, in conditions appropriate
to a Type Ia supernovae. The domain is 2 m x 4 m.
Scientific Calculations:
J.B. Bell, C.A. Rendleman, and M.S. Day, Lawrence Berkeley National Laboratory;
S.E. Woosley and M. Zingale, University of California, Santa Cruz
The Propagation and Eruption of Relativistic Jets from the Stellar
Progenitors of Gamma Ray Bursts
Movie (9.2 MB MPEG)
Description:
Recent findings support the "collapsar" model for the production
of gamma ray bursts. In this model the core of a massive star
collapses into a black hole.
New two- and three-dimensional calculations on NERSC IBM SP,
Seaborg, show the break-out of so-called "relativistic jets" as
they erupt from the surface of the parent star.
This computer simulation shows the distribution of relativistic particles
in a jet as it breaks out of the star. Yellow and orange are very high
energy and will ultimately make a gamma ray burst.
Scientific Calculations:
Weiqun Shang, S.E. Woosley, University of California, Santa
Cruz, and A. Heger, Los Alamos National Laboratory
Star Formation and Stellar Emission in Simulations of Interacting Galaxies
Description:
This video shows the projected gas density in the
collision and merger of two
disk galaxies. The cacluations were performed using
galaxy models based upon observations of local
spiral galaxies placed on cosmologically realistic
orbit and evolved using the n-body/SPH (smoothed
particle hydrodynamics) code GADGET.
Description:
This movie shows a collision similar to the previous one,
but the results are processed through a radiative transfer
code to account for emission of stellar light and absorption
by interstellar dust, in order to produce
images comparable to what would be measured by observations.
Scientific Calculations and Visualizations:
T.J. Cox1, Patrik Jonsson, and Joel Primack, University of
California, Santa Cruz, and 1Harvard Center for
Astrophysics
Terascale Supernova Initiative: Simulations of Type II Supernova
Explosions
Description:
This video shows how the entropy structure relates to convection below
the neutrinosphere.
Scientific Calculations:
Doug Swesty and Eric Myra, State University of New York, Stony Brook
Description:
This video illustrates
both the magnitude and direction of the fluid flow in the same
epoch.
Visualizations:
Polly Baker and Ed Bachta, University of Indiana
Rayleigh-Taylor Unstable Flames in a Type Ia Supernova