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The mitigating effect of magnetic fields on Rayleigh-Taylor unstable inertial confinement fusion plasmasa)
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10.1063/1.4803092
/content/aip/journal/pop/20/5/10.1063/1.4803092
http://aip.metastore.ingenta.com/content/aip/journal/pop/20/5/10.1063/1.4803092
View: Figures

Figures

Image of FIG. 1.
FIG. 1.

(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.

Image of FIG. 2.
FIG. 2.

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.

Image of FIG. 3.
FIG. 3.

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.

Image of FIG. 4.
FIG. 4.

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.

Image of FIG. 5.
FIG. 5.

Fluid density (a), (b), (c), and (d) for late-time multimode using a seed magnetic field of 10 T.

Image of FIG. 6.
FIG. 6.

Multimode plot of peak magnetic field vs bubble position (a) for each of the in-plane ( ) and out-of-plane () magnetic fields. Plot (b) plots the minimum plasma beta as a function of bubble position.

Image of FIG. 7.
FIG. 7.

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.

Image of FIG. 8.
FIG. 8.

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), (c), (d), and (e).

Image of FIG. 9.
FIG. 9.

Peak magnetic fields, out-of-plane 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.

Image of FIG. 10.
FIG. 10.

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 .

Image of FIG. 11.
FIG. 11.

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 .

Image of FIG. 12.
FIG. 12.

Fluid vorticity spectrum for solutions with different seed in-plane magnetic fields at the same bubble positions, (a) and (b).

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/content/aip/journal/pop/20/5/10.1063/1.4803092
2013-04-29
2014-04-17
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752b84549af89a08dbdd7fdb8b9568b5 journal.articlezxybnytfddd
Scitation: The mitigating effect of magnetic fields on Rayleigh-Taylor unstable inertial confinement fusion plasmas<sup>a)</sup>
http://aip.metastore.ingenta.com/content/aip/journal/pop/20/5/10.1063/1.4803092
10.1063/1.4803092
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