Diagnosing Plasma Gradients Using Spectral Line Shapes [electronic resource]

The development of a set of stable implosions using indirectly driven plastic microspheres with argon (0.1 atm) doped deuterium (50 atm) has provided a unique source for testing the plasma spectroscopy of the high energy density imploded core. The core reaches electron densities of > 10²⁴ cm⁻³ wi...

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Bibliographic Details
Online Access: Online Access (via OSTI)
Corporate Author: Lawrence Berkeley National Laboratory (Researcher)
Format: Government Document Electronic eBook
Language:English
Published: Washington, D.C. : Oak Ridge, Tenn. : United States. Department of Energy. ; distributed by the Office of Scientific and Technical Information, U.S. Department of Energy, 2000.
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Summary:The development of a set of stable implosions using indirectly driven plastic microspheres with argon (0.1 atm) doped deuterium (50 atm) has provided a unique source for testing the plasma spectroscopy of the high energy density imploded core. The core reaches electron densities of > 10²⁴ cm⁻³ with temperatures of ≈ 1 keV and has been shown to be reproducible on a shot to shot basis. Moreover, it has been shown that not only the peak temperature and density are consistent, but that the temporal evolution of the mean temperature and density of the final phase of the implosion is also reproducible. These imploding cores provide a unique opportunity to test aspects of plasma spectroscopy that are difficult to study in other plasmas and to develop methods to test stable hydrodynamics. We present experimental results and discuss spectroscopic analysis algorithms to determine consistent temperature and density fits to determine gradients in the plasma.
Item Description:Published through SciTech Connect.
11/13/2000.
"ucrl-jc-139309"
559 ISSN 0094-243X.
15th International Conference on Spectral Line Shapes, Berlin, Germany, Jul 10 - Jul 14, 2000.
Back, C A; Golovkin, I; Mancini, R; Missalla, T; Landen, O L; Lee, R W; Klein, L.
Physical Description:14p : digital, PDF file.