Interface imprinting by a rippled shock using an intense laser

Kane, J.; Robey, H. F.; Remington, B. A.; Drake, R. P.; Knauer, J.P.; Ryutov, D. D.; Louis, H.; Teyssier, Romain; Hurricane, O. A.; Arnett, David; Rosner, R.; Calder, A. C.

doi:10.1103/physreve.63.055401

Cited by 61 publications

(31 citation statements)

References 22 publications

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“…An extension of our calculations to three dimensions with a similar resolution as in the 2D case appears hardly feasible in view of present computer resources. Further insight might, however, be gained by laser experiments Kane et al 2001;Drake et al 2002;Klein et al 2003, and the references therein), and hydrodynamic code validation experiments as those described by Fishbine (2002) and Zoldi (2002) before well-resolved 3D hydrodynamic simulations will become available.…”

Section: Discussionmentioning

confidence: 99%

Non-spherical core collapse supernovae

Kifonidis

Plewa

Janka

et al. 2003

A&A

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Abstract.We have performed two-dimensional simulations of core collapse supernovae that encompass shock revival by neutrino heating, neutrino-driven convection, explosive nucleosynthesis, the growth of Rayleigh-Taylor instabilities, and the propagation of newly formed metal clumps through the exploding star. A simulation of a type II explosion in a 15 M blue supergiant progenitor is presented, that confirms our earlier type II models and extends their validity to times as late as 5.5 hours after core bounce. We also study a type Ib-like explosion, by simply removing the hydrogen envelope of the progenitor model. This allows for a first comparison of type II and type Ib evolution. We present evidence that the hydrodynamics of core collapse supernovae beyond shock revival differs markedly from the results of simulations that have followed the Rayleigh-Taylor mixing starting from ad hoc energy deposition schemes to initiate the explosion. We find iron group elements to be synthesized in an anisotropic, dense, low-entropy shell that expands with velocities of ∼17 000 km s −1 shortly after shock revival. The growth of Rayleigh-Taylor instabilities at the Si/O and (C+O)/He composition interfaces of the progenitor, seeded by the flow-structures resulting from neutrino-driven convection, leads to a fragmentation of this shell into metal-rich "clumps". This fragmentation starts already ∼20 s after core bounce and is complete within the first few minutes of the explosion. During this time the clumps are slowed down by drag, and by the positive pressure gradient in the unstable layers. However, at t ≈ 300 s they decouple from the flow and start to propagate ballistically and subsonically through the He core, with the maximum velocities of metals remaining constant at ∼3500−5500 km s −1 . This early "clump decoupling" leads to significantly higher 56 Ni velocities at t = 300 s than in one-dimensional models of the explosion, demonstrating that multi-dimensional effects which are at work within the first minutes, and which have been neglected in previous studies (especially in those which dealt with the mixing in type II supernovae), are crucial. Despite comparably high initial maximum nickel velocities in both our type II and our type Ib-like model, we find that there are large differences in the final maximum nickel velocities between both cases. In the "type Ib" model the maximum velocities of metals remain frozen in at ∼3500−5500 km s −1 for t ≥ 300 s, while in the type II model they drop significantly for t > 1500 s. In the latter case, the massive hydrogen envelope of the progenitor forces the supernova shock to slow down strongly, leaving behind a reverse shock and a dense helium shell (or "wall") below the He/H interface. After penetrating into this dense material the metal-rich clumps possess supersonic speeds, before they are slowed down by drag forces to ∼1200 km s −1 at a time of 20 000 s post-bounce. While, due to this deceleration, the maximum velocities of iron-group elements in SN 1987 A cannot be reproduced ...

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Section: Discussionmentioning

confidence: 99%

Non-spherical core collapse supernovae

Kifonidis

Plewa

Janka

et al. 2003

A&A

303

330

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“…II. Adapted from Kane et al, 2001. ͑b͒ The experimental radiograph at 39 ns ͑bottom͒ and 65 ns ͑top͒ for the experiment corresponding to the design simulation shown in ͑a͒.…”

Section: E Experiments On Sn Type-ii Hydrodynamicsmentioning

confidence: 99%

Experimental astrophysics with high power lasers andZpinches

2006

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With the advent of high-energy-density ͑HED͒ experimental facilities, such as high-energy lasers and fast Z-pinch, pulsed-power facilities, millimeter-scale quantities of matter can be placed in extreme states of density, temperature, and/or velocity. This has enabled the emergence of a new class of experimental science, HED laboratory astrophysics, wherein the properties of matter and the processes that occur under extreme astrophysical conditions can be examined in the laboratory. Areas particularly suitable to this class of experimental astrophysics include the study of opacities relevant to stellar interiors, equations of state relevant to planetary interiors, strong shock-driven nonlinear hydrodynamics and radiative dynamics relevant to supernova explosions and subsequent evolution, protostellar jets and high Mach number flows, radiatively driven molecular clouds and nonlinear photoevaporation front dynamics, and photoionized plasmas relevant to accretion disks around compact objects such as black holes and neutron stars.

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“…Asymmetric irradiation and/or rough surface finishes can lead to a nonuniform ablation process, and thus to the generation of perturbed shock waves. The presence of distorted fronts in ICF pellets is significant because of their potential for seeding hydrodynamic instabilities (via "interface imprinting" [9] or otherwise [10]), which disturb uniform highdensity compression and reduce gain. A better understanding of the dynamics of perturbed shocks in real materials could provide insight into how to suppress these instabilities, thus improving the overall uniformity of the compression process.…”

Section: Introductionmentioning

confidence: 99%

Initial-value-problem solution for isolated rippled shock fronts in arbitrary fluid media

Bates

2004

Phys. Rev. E

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Following the work of Roberts (Los Alamos Scientific Laboratory Report No. LA-299, 1945), we investigate the effect of small two-dimensional perturbations on an isolated, planar shock front moving steadily through an inviscid fluid medium with an arbitrary equation of state (EOS). In the context of an initial-value problem, we derive explicit analytical expressions for the linearized, time-dependent Fourier coefficients associated with an initial corrugation of the front. The temporal evolution of these coefficients superficially resembles the attenuated "ringing" of a damped harmonic oscillator, but with the important distinctions that the frequency of oscillation is not constant, and that the damping factor is not simply an exponential function of time t. It is shown that at least two three-parameter families of stable solutions exist, one more strongly damped than the other. In both cases, we find that the envelope of oscillations decays asymptotically as t −3/2 , with shorter wavelengths dying out earlier than longer ones. For a particular perturbedshock system, the strength of the front and the EOS properties of the material through which it propagates determine the applicable family of solutions. Theoretical predictions agree well with FAST2D numerical simulations for several examples derived from the CALEOS library. Public reporting burden for the collection of information is estimated to average 1 hour per response, including the time for reviewing instructions, searching existing data sources, gathering and maintaining the data needed, and completing and reviewing the collection of information. Send comments regarding this burden estimate or any other aspect of this collection of information, including suggestions for reducing this burden, to Washington Headquarters Services, Directorate for Information Operations and Reports, 1215 Jefferson Davis Highway, Suite 1204, Arlington VA 22202-4302. Respondents should be aware that notwithstanding any other provision of law, no person shall be subject to a penalty for failing to comply with a collection of information if it does not display a currently valid OMB control number. In the context of an initial-value problem, we derive explicit analytical expressions for the linearized, time-dependent Fourier coefficients associated with an initial corrugation of the front. The temporal evolution of these coefficients superficially resembles the attenuated inging" of a damped harmonic oscillator, but with the important distinctions that the frequency of oscillation is not constant, and that the damping factor is not simply an exponential function of time t. It is shown that at least two three-parameter families of stable solutions exist, one more strongly damped than the other. In both cases, we find that the envelope of oscillations decays asymptotically as t-3=2, with shorter wavelengths dying out earlier than longer ones. For a particular perturbedshock system, the strength of the front and the EOS properties of the material through which it propagates d...

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Interface imprinting by a rippled shock using an intense laser

Cited by 61 publications

References 22 publications

Non-spherical core collapse supernovae

Non-spherical core collapse supernovae

Experimental astrophysics with high power lasers andZpinches

Initial-value-problem solution for isolated rippled shock fronts in arbitrary fluid media

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