(perpendicular electron thermal conductivity) as a function of (electron magnetization) for ICF relevant parameters (density and temperature) to determine the effect of electron magnetization on electron thermal conductivity.
Density (a) and out-of-plane self-generated magnetic field (b) for a single-mode RTI. Self-generated out-of-plane magnetic fields are appropriately aligned for mitigating thermal loss from the hot-spot.
Density evolution in the presence of a large external in-plane magnetic field (a), the magnitude of the MHD dynamo amplified in-plane magnetic fields (b), and the vector plot of the MHD dynamo amplified in-plane magnetic fields (c). The initially uniform external magnetic fields become appropriately aligned for mitigating thermal loss from the hot-spot.
Multimode peak magnetic field, magnetic flux over entire domain, and normalized vorticity are plotted in (a), and plasma is plotted in (b) as a function of the bubble position.
Fluid density (a), Bx (b), By (c), and Bz (d) for late-time multimode using a seed magnetic field of 10 T.
Multimode plot of peak magnetic field vs bubble position (a) for each of the in-plane ( ) and out-of-plane (Bz ) magnetic fields. Plot (b) plots the minimum plasma beta as a function of bubble position.
Multimode plots of fluid density with no seed magnetic field (a) and with a 10 T seed magnetic field at the onset of deceleration (b). Plot (c) estimates the minimum external seed magnetic field (6 T oriented at 45° at the onset of deceleration) below which there is no further thermal conduction mitigation compared to the self-generated magnetic fields.
Late-time multimode fluid density with no seed magnetic field (a), and late-time multimode plots using a seed magnetic field of 1000 T of fluid density (b), Bx (c), By (d), and Bz (e).
Peak magnetic fields, out-of-plane Bz and in-plane , as a function of bubble position is shown in plot (a). from Eq. (19) is plotted in (b) as a function of the peak in-plane magnetic fields. Note that the in-plane fields get to much larger magnitudes than the out-of-plane magnetic fields.
Bubble position as a function of time (a) and plasma as a function of the bubble position (b) for several seed in-plane magnetic fields. Note that large magnetic fields lead to slower RTI bubble growth as well as much smaller plasma .
Comparing orientation of seed magnetic field transverse to the interface (a) and normal to the interface (b) after the bubble/spike have traveled the same distance as Fig. 8 .
Fluid vorticity spectrum for solutions with different seed in-plane magnetic fields at the same bubble positions, (a) and (b).
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