Energy Deposition, Penetration, Blooming of Energetic Electrons in Fast Ignition and Preheat Scenarios

Details Energy Deposition, Penetration, Blooming of Energetic Electrons in Fast Ignition and Preheat Scenarios Energy Deposition, Penetration, Blooming of Energetic Electrons in Fast Ignition and Preheat Scenarios

Oct 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005aps..dppgo1005p&link_type=abstract

American Physical Society, 47th Annual DPP Meeting, October 24-28, 2005, abstract #GO1.005

Astronomy and Astrophysics

Astrophysics

Scientific paper

For plasmas of arbitrary Z and density, the penetration, energy deposition, blooming, and straggling of energetic electrons are analytically modeled. Calculations spanning 25 orders of magnitude in density apply to fast ignition (n˜10^26/cc), electron preheat (n˜10^23/cc) and relativistic astrophysical jets (n˜ 10/cc). It is shown that ρ, the product of density and linear penetration, is a basic parameter and that blooming and straggling have a strong Z dependence. For fast-ignition with 1-MeV electrons in DT plasma, ρ = 0.42 g/cm^2 , = 14 μm and bloom = 5 μm; the blooming-to-penetration ratio is 0.35; in Cu (Z=29) plasma of the same electron density, the ratio is 1.1. For preheat with 100 keV electrons in DT ice, ρ = 0.007 g/cm^2 , = 280 μm, close to the 300-μm ice-layer thickness prescribed for NIF direct-drive designs. For the astrophysical jet, ρ = 0.42 g/cm^2 and ˜ 10^4 light years. These calculations will be used to establish requirements for fast ignition and tolerable levels of electron preheat for ICF targets. This work was supported in part by LLE, LLNL, the U.S. DoE, the Univ. of Rochester Fusion Science Center.

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