2008 APS April Meeting and HEDP/HEDLA Meeting
Volume 53, Number 5
Friday–Tuesday, April 11–15, 2008;
St. Louis, Missouri
Session 1HE: Stellar Explosions, Turbulence and Instabilities
8:30 AM–11:15 AM,
Friday, April 11, 2008
Hyatt Regency St. Louis Riverfront (formerly Adam's Mark Hotel),
Room: Promenade F
Sponsoring
Units:
HEDP HEDLA
Chair: Paul Drake, University of Michigan
Abstract ID: BAPS.2008.APR.1HE.4
Abstract: 1HE.00004 : Laboratory blast wave driven instabilities
9:45 AM–10:10 AM
Preview Abstract
Abstract
Author:
Carolyn Kuranz
(University of Michigan)
This presentation discusses experiments well-scaled to the blast
wave driven
instabilities during the explosion phase of SN1987A. Blast waves
occur
following a sudden, finite release of energy, and consist of a
shock front
followed by a rarefaction wave. When a blast wave crosses an
interface with
a decrease in density, hydrodynamic instabilities will develop.
These
experiments include target materials scaled in density to the
He/H layer in
SN1987A. About 5 kJ of laser energy from the Omega Laser facility
irradiates
a 150 $\mu $m plastic layer that is followed by a low density
foam layer. A
blast wave structure similar to those in supernovae, is created
in the
plastic layer. The blast wave crosses a perturbed interface,
which produces
nonlinear, unstable growth dominated by the Rayleigh-Taylor (RT)
instability. Recent experiments have been performed using complex
initial
conditions featuring a three-dimensional interface structure with a
wavelength of 71 $\mu $m in two orthogonal directions, at times
supplemented
by an additional sinusoidal mode of 212 $\mu $m or 424 $\mu $m.
We have
detected the interface structure under these conditions, using dual
orthogonal radiographs on some shots, and will show some of the
resulting
data. Recent advancements in our x-ray backlighting techniques
have greatly
improved the resolution of our x-ray radiographic images. Under
certain
conditions, the improved images show some mass extending beyond
the RT spike
and penetrating further than previously observed. Current
simulations do not
show this phenomenon. This presentation will discuss the amount
of mass in
these spike extensions as well as the error analysis of this
calculation.
Future experiments will also be discussed. They will be focusing on
realistic initial conditions based on 3D stellar evolution models.
This research was sponsored by the Stewardship Science Academic
Alliances
Program through DOE Research Grants DE-FG52-07NA28058,
DE-FG52-04NA00064,
and other grants and contracts.
To cite this abstract, use the following reference: http://meetings.aps.org/link/BAPS.2008.APR.1HE.4