Radiation Transport in High Energy Density Plasma

Details Radiation Transport in High Energy Density Plasma Radiation Transport in High Energy Density Plasma

Apr 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002aps..apr.k7003s&link_type=abstract

American Physical Society, April Meeting, Jointly Sponsored with the High Energy Astrophysics Division (HEAD) of the American As

Astronomy and Astrophysics

Astrophysics

Scientific paper

Accurate models for the radiative properties of hot, dense matter are crucial to understanding systems ranging from stellar interiors to inertial confinement fusion (ICF) plasmas. Models for photo-absorption are complex, requiring knowledge of atomic structure, transition strengths, level populations, spectral line shapes, and plasma interactions. For such systems, detailed approaches accounting for all bound levels in a consistent thermodynamic model for equation of state (EOS) can require an enormous quantity of atomic data, beyond the computational capabilities of current supercomputers. Exact treatments of the many-body ion plasma effects remain insoluble, and significant uncertainties may persist due to computational methods regarding the role of the high density EOS. In addition, the extension to non-equilibrium models is required for both ICF and astrophysical plasma, requiring knowledge of detailed kinetics. Simplifying assumptions and approximations are often used including: truncations of the atomic data set treated in detail or at all, the use of arbitrary cut-offs for plasma effects, and the use of mean field approximations, or statistical methods to simplify the treatment for complex configurations. Given their complexity and widespread use, it is essential to test radiative opacity models in well-characterized laboratory experiments. Using new techniques and instrumentation, we have accurately measured the frequency dependent absorption of well-characterized, radiatively heated plasmas, to test both equilibrium and non-equilibrium models. Different experimental venues allowed plasma conditions to vary over many orders of magnitude, overlapping conditions of interest to fusion targets, stellar envelopes, and accretion disk plasmas. The relevant plasma conditions, density, temperature and radiation environment are independently measured, allowing detailed comparison with opacity and radiative plasma theory. The experiments demonstrate the accuracy and range of validity of several opacity models having a variety of approximations in the atomic physics, equation of state, and computational methodologies. This work was performed under the auspices of the U.S. Department of Energy by the University of California, Lawrence Livermore National Laboratory under contract No. W-7405-Eng-48.

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