Observations of Multiple Nuclear Reaction Histories and Fuel-Ion Species Dynamics in Shock-Driven Inertial Confinement Fusion Implosions

Fuel-ion species dynamics in hydrodynamiclike shock-driven DT^{3}He-filled inertial confinement fusion implosion is quantitatively assessed for the first time using simultaneously measured D^{3}He and DT reaction histories. These reaction histories are measured with the particle x-ray temporal diagn...

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Veröffentlicht in:Physical review letters 2019-01, Vol.122 (3), p.035001-035001, Article 035001
Hauptverfasser: Sio, H, Frenje, J A, Le, A, Atzeni, S, Kwan, T J T, Gatu Johnson, M, Kagan, G, Stoeckl, C, Li, C K, Parker, C E, Forrest, C J, Glebov, V, Kabadi, N V, Bose, A, Rinderknecht, H G, Amendt, P, Casey, D T, Mancini, R, Taitano, W T, Keenan, B, Simakov, A N, Chacón, L, Regan, S P, Sangster, T C, Campbell, E M, Seguin, F H, Petrasso, R D
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Sprache:eng
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Zusammenfassung:Fuel-ion species dynamics in hydrodynamiclike shock-driven DT^{3}He-filled inertial confinement fusion implosion is quantitatively assessed for the first time using simultaneously measured D^{3}He and DT reaction histories. These reaction histories are measured with the particle x-ray temporal diagnostic, which captures the relative timing between different nuclear burns with unprecedented precision (∼10  ps). The observed 50±10  ps earlier D^{3}He reaction history timing (relative to DT) cannot be explained by average-ion hydrodynamic simulations and is attributed to fuel-ion species separation between the D, T, and ^{3}He ions during shock convergence and rebound. At the onset of the shock burn, inferred ^{3}He/T fuel ratio in the burn region using the measured reaction histories is much higher as compared to the initial gas-filled ratio. As T and ^{3}He have the same mass but different charge, these results indicate that the charge-to-mass ratio plays an important role in driving fuel-ion species separation during strong shock propagation even for these hydrodynamiclike plasmas.
ISSN:0031-9007
1079-7114
DOI:10.1103/PhysRevLett.122.035001