Secondary shock formation in xenon-nitrogen mixtures

Hansen, J. F.; Edwards, M. J.; Froula, D. H.; Edens, Aaron; Gregori, G.; Ditmire, T.

doi:10.1063/1.2359283

Cited by 7 publications

(11 citation statements)

References 28 publications

(31 reference statements)

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“…29. The secondary shock has been attributed the heat wave, which outran the radiative shock in this experiment.…”

Section: Discussionmentioning

confidence: 99%

“…Our simulation would cover a time scale of about 50 ps, which is more than three orders of magnitude shorter than the lifetime of the second shock in Ref. 29. A lower ionization state of the nitrogen and the presence of neutral nitrogen would reduce the ion plasma frequency and extend the life-time of the secondary shock.…”

Section: Discussionmentioning

confidence: 99%

“…Let us consider the case study in Ref. 29, where the residual gas consists entirely of nitrogen and we furthermore assume that the nitrogen is fully ionized. We obtain an ion plasma frequency x i % 3 Â 10 12 s À1 .…”

Section: Discussionmentioning

confidence: 99%

“…The residual gas in Ref. 29 consisted of a mixture of Xenon and Nitrogen gas with a mass density of 3:6 Â 10 À5 g cm À3 . Let us consider the case study in Ref.…”

Section: Discussionmentioning

confidence: 99%

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Shocks in unmagnetized plasma with a shear flow: Stability and magnetic field generation

et al. 2015

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A pair of curved shocks in a collisionless plasma is examined with a two-dimensional particle-incell (PIC) simulation. The shocks are created by the collision of two electron-ion clouds at a speed that exceeds everywhere the threshold speed for shock formation. A variation of the collision speed along the initially planar collision boundary, which is comparable to the ion acoustic speed, yields a curvature of the shock that increases with time. The spatially varying Mach number of the shocks results in a variation of the downstream density in the direction along the shock boundary. This variation is eventually equilibrated by the thermal diffusion of ions. The pair of shocks is stable for tens of inverse ion plasma frequencies. The angle between the mean flow velocity vector of the inflowing upstream plasma and the shock's electrostatic field increases steadily during this time. The disalignment of both vectors gives rise to a rotational electron flow, which yields the growth of magnetic field patches that are coherent over tens of electron skin depths.

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“…29. The secondary shock has been attributed the heat wave, which outran the radiative shock in this experiment.…”

Section: Discussionmentioning

confidence: 99%

Section: Discussionmentioning

confidence: 99%

Section: Discussionmentioning

confidence: 99%

“…The residual gas in Ref. 29 consisted of a mixture of Xenon and Nitrogen gas with a mass density of 3:6 Â 10 À5 g cm À3 . Let us consider the case study in Ref.…”

Section: Discussionmentioning

confidence: 99%

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Shocks in unmagnetized plasma with a shear flow: Stability and magnetic field generation

et al. 2015

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“…The degree of collisionality in a laboratory plasma experiment depends on the intensity of the laser pulse and on the observational time scale. Hansen et al (2006) observed a collisional shock.…”

Section: The Hybrid Structure and Related Experimentsmentioning

confidence: 99%

The interplay of the collisionless non-linear thin-shell instability with the ion acoustic instability

Dieckmann

Folini

Walder

2016

Mon. Not. R. Astron. Soc.

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The nonlinear thin-shell instability (NTSI) may explain some of the turbulent hydrodynamic structures that are observed close to the collision boundary of energetic astrophysical outflows. It develops in nonplanar shells that are bounded on either side by a hydrodynamic shock, provided that the amplitude of the seed oscillations is sufficiently large. The hydrodynamic NTSI has a microscopic counterpart in collisionless plasma. A sinusoidal displacement of a thin shell, which is formed by the collision of two clouds of unmagnetized electrons and protons, grows and saturates on timescales of the order of the inverse proton plasma frequency. Here we increase the wavelength of the seed perturbation by a factor 4 compared to that in a previous study. Like in the case of the hydrodynamic NTSI, the increase in the wavelength reduces the growth rate of the microscopic NTSI. The prolonged growth time of the microscopic NTSI allows the waves, which are driven by the competing ion acoustic instability, to grow to a large amplitude before the NTSI saturates and they disrupt the latter. The ion acoustic instability thus imposes a limit on the largest wavelength that can be destabilized by the NTSI in collisionless plasma. The limit can be overcome by binary collisions. We bring forward evidence for an overstability of the collisionless NTSI.

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Simulations of radiative effects on the Rayleigh–Taylor instability using the CRASH code

Trantham¹,

Kuranz²,

Malamud³

et al. 2013

High Energy Density Physics

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Secondary shock formation in xenon-nitrogen mixtures

Cited by 7 publications

References 28 publications

Shocks in unmagnetized plasma with a shear flow: Stability and magnetic field generation

Shocks in unmagnetized plasma with a shear flow: Stability and magnetic field generation

The interplay of the collisionless non-linear thin-shell instability with the ion acoustic instability

Simulations of radiative effects on the Rayleigh–Taylor instability using the CRASH code

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