How high energy fluxes may affect Rayleigh–Taylor instability growth in young supernova remnants

Kuranz, Carolyn; Park, H.-S.; Huntington, C. M.; Miles, A. R.; Remington, B. A.; Plewa, T.; Trantham, Matthew; Robey, H. F.; Shvarts, D.; Shimony, A.; Raman, Kumar; MacLaren, S. A.; Wan, Weigang; Doss, F. W.; Kline, J. L.; Flippo, Kirk; Malamud, G.; Handy, Timothy; Prisbrey, Shon; Krauland, C.; Klein, Sallee; Harding, Eric; Wallace, R. J.; Grosskopf, M.J.; Marion, D.C.; Kalantar, D. H.; Giraldez, E.; Drake, R. P.

doi:10.1038/s41467-018-03548-7

Cited by 108 publications

(51 citation statements)

References 18 publications

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“…We note, that one dimensional simulations, in which no energy is lost to the walls and where the wall ablation is not present, show no such slowing. We also note, that similar phenomena were observed in previous hydrodynamic experiments [41,42].…”

Section: B 2d Corrections To the 1d Estimationsupporting

confidence: 91%

Key to understanding supersonic radiative Marshak waves using simple models and advanced simulations

Cohen¹,

Malamud

Heizler³

2020

Phys. Rev. Research

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This article studies the propagation of supersonic radiative Marshak waves. These waves are radiation dominated, and play an important role in inertial confinement fusion and in astrophysical and laboratory systems. For that reason, this phenomenon has attracted considerable experimental attention in recent decades in several different facilities. The present study integrates the various experimental results published in the literature, demonstrating a common physical base. A new simple semi-analytic model, is derived and presented along with advanced radiative hydrodynamic implicit Monte Carlo direct numerical simulations, which explain the experimental results. This study identifies the main physical effects dominating the experiments, notwithstanding their different apparatuses and different physical regimes. *

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Section: B 2d Corrections To the 1d Estimationsupporting

confidence: 91%

Key to understanding supersonic radiative Marshak waves using simple models and advanced simulations

Cohen¹,

Malamud

Heizler³

2020

Phys. Rev. Research

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“…4 A ). This creates a strong source of radiation from the radiative shock in the SiO 2 foam which can reduce the perturbation growth at the plastic–foam interface by ablative stabilization (52–54). A radiation cavity (hohlraum, 4 mm diameter × 3 mm long, shown in Fig.…”

Section: Radiative Shock Stabilization Of Planar Hydrodynamic Instabimentioning

confidence: 99%

Rayleigh–Taylor instabilities in high-energy density settings on the National Ignition Facility

Remington

Park

Casey

et al. 2018

Proc. Natl. Acad. Sci. U.S.A.

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The Rayleigh-Taylor (RT) instability occurs at an interface between two fluids of differing density during an acceleration. These instabilities can occur in very diverse settings, from inertial confinement fusion (ICF) implosions over spatial scales of [Formula: see text] cm (10-1,000 μm) to supernova explosions at spatial scales of [Formula: see text] cm and larger. We describe experiments and techniques for reducing ("stabilizing") RT growth in high-energy density (HED) settings on the National Ignition Facility (NIF) at Lawrence Livermore National Laboratory. Three unique regimes of stabilization are described: () at an ablation front, () behind a radiative shock, and () due to material strength. For comparison, we also show results from nonstabilized "classical" RT instability evolution in HED regimes on the NIF. Examples from experiments on the NIF in each regime are given. These phenomena also occur in several astrophysical scenarios and planetary science [Drake R (2005) 47:B419-B440; Dahl TW, Stevenson DJ (2010) 295:177-186].

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“…Provided the scalability can be established, numerical simulations of the laboratory experiment with controlled initial conditions (which one can vary on the shot-to-shot basis) and numerous diagnostics, establishes a firm base for the code validation and verification. It is this area where considerable effort has been spent during the past decade (e.g., Calder et al, 2002Calder et al, , 2004Valarde et al, 2006;Stehle et al, 2009;Kuranz et al, 2010Kuranz et al, , 2018.…”

Section: Agn -Active Galactic Nucleimentioning

confidence: 99%

Exploring astrophysics-relevant magnetohydrodynamics with pulsed-power laboratory facilities

2019

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Laboratory facilities employing high pulsed currents and voltages, and called generally "pulsed-power facilities", allow experimenters to produce a variety of hydrodynamical structures replicating, often in a scalable fashion, a broad range of dynamical astrophysical phenomena. Among these are: astrophysical jets and outflows, astrophysical blast waves, magnetized radiatively dominated flows and, more recently, aspects of simulated accretion disks. The magnetic field thought to play significant role in most of the aforementioned objects is naturally present and controllable in pulsed-power environments. The size of the objects produced in pulsed-power experiments ranges from a centimeter to tens of centimeters, thereby allowing the use of a variety of diagnostic techniques. In a number of situations astrophysical morphologies can be replicated down to the finest structures. The configurations and their parameters are highly reproducible; one can vary them to isolate the most important phenomena and thereby help in developing astrophysical models. This approach has emerged as a useful tool in the quest to better understand magnetohydrodynamical effects in astronomical environments. The present review summarizes the progress made during the last decade and is designed to help readers identify and, perhaps, implement new experiments in this growing research area. Techniques used for generation and characterization of the flows are described. 1 Retired 2 CONTENTS I. Introduction II. Jets and outflows-weak magnetic field A. Generating plasma streams and plasma jets with wire arrays. B. Hypersonic, radiatively cooled hydrodynamic jets and their interaction with the ambient medium C. Hydrodynamic interaction of the jets with a side wind D. Highly-collimated jets produced by ablation of the central area of a metal foil III. Jets and outflows-significant magnetic field A. Magnetically-dominated tower jets B. Formation of energetic ions in a magnetic cavity C. Possible role of axial magnetic field B. Episodic events and internal shocks E. Magnetic arches and their stability F. MHD equilibria stabilized by the shear flow IV. Rotating plasmas-on the way to imitating the accretion discs V. Shock waves A. General comments B. Blast waves and radiative precursors C. Shocks in the colliding streams D. Introducing magnetic field E. Interaction of magnetized streams with clumps and globules VI. Non-MHD effects A. Hall and other two-fluid effects B. Generation of energetic particles C.

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How high energy fluxes may affect Rayleigh–Taylor instability growth in young supernova remnants

Cited by 108 publications

References 18 publications

Key to understanding supersonic radiative Marshak waves using simple models and advanced simulations

Key to understanding supersonic radiative Marshak waves using simple models and advanced simulations

Rayleigh–Taylor instabilities in high-energy density settings on the National Ignition Facility

Exploring astrophysics-relevant magnetohydrodynamics with pulsed-power laboratory facilities

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