Dynamical Overstability of Radiative Blast Waves: The Atomic Physics of Shock Stability

Laming, J. M.; Grün, J.

doi:10.1103/physrevlett.89.125002

Cited by 59 publications

(47 citation statements)

References 37 publications

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“…This was attributed to the lateral radiation losses (through the walls of the shock tube), which reduce the amount of radiation heating the precursor and thus affect its structure (Leygnac et al 2006;González et al 2006b). Keilty et al (2000), Shigemori et al (2000), Edwards et al (2001), Calder et al (2002, and Laming & Grun (2002) focused their studies on the spherical, radiative, blast waves, which are similar to those studied in the previous 1D cases, in terms of the development of radiative precursor, but also exhibit strong differences, such as the importance of radiative cooling and the development of various instabilities. The study of these experimental blast waves is linked to the problem of the evolution and stability of supernova remnants.…”

Section: Introductionmentioning

confidence: 99%

2D numerical study of the radiation influence on shock structure relevant to laboratory astrophysics

González

Audit

Stehlé

2009

A&A

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Context. Radiative shocks are found in various astrophysical objects and particularly at different stages of stellar evolution. Studying radiative shocks, their topology, and thermodynamical properties is therefore a starting point to understanding their physical properties. This study has become possible with the development of large laser facilities, which has provided fresh impulse to laboratory astrophysics. Aims. We present the main characteristics of radiative shocks modeled using cylindrical simulations. We focus our discussion on the importance of multi-dimensional radiative-transfer effects on the shock topology and dynamics. Methods. We present results obtained with our code HERACLES for conditions corresponding to experiments already performed on laser installations. The multi-dimensional hydrodynamic code HERACLES is specially adapted to laboratory astrophysics experiments and to astrophysical situations where radiation and hydrodynamics are coupled. Results. The importance of the ratio of the photon mean free path to the transverse extension of the shock is emphasized. We present how it is possible to achieve the stationary limit of these shocks in the laboratory and analyze the angular distribution of the radiative flux that may emerge from the walls of the shock tube. Conclusions. Implications of these studies for stellar accretion shocks are presented.

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Section: Introductionmentioning

confidence: 99%

2D numerical study of the radiation influence on shock structure relevant to laboratory astrophysics

González

Audit

Stehlé

2009

A&A

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“…22,23 Such instability has indeed been observed in laser-driven experiments with strongly radiating gases, 24 see also Refs. 25,26 and references therein.…”

Section: Introductionmentioning

confidence: 99%

“…For example, for spherical geometry one more real eigenvalue exists for 2 γ > and two more for 1.5565 2 γ < < , see the Table. Similarly, for the perturbations with 1 l = or 1 m = there always exists one real eigenvalue σ ν = − corresponding to a sonic eigenmode for which the entropic perturbation vanishes, cf. (26). But since this mode is not radial, the vortical contribution represented by the second term in the right-hand side of (27) …”

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confidence: 99%

Stability of stagnation via an expanding accretion shock wave

et al. 2016

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Stagnation of a cold plasma streaming to the center or axis of symmetry via an expanding accretion shock wave is ubiquitous in inertial confinement fusion (ICF) and high-energy- (2014)]. Some experimental evidence indicates that stagnation via an expanding shock wave is stable, but its stability has never been studied theoretically. We present such analysis for the stagnation that does not involve a rarefaction wave behind the expanding shock front and is described by the classic ideal-gas Noh solution in spherical and cylindrical geometry. In either case the stagnated flow has been demonstrated to be stable, initial perturbations exhibiting a powerlaw, oscillatory or monotonic, decay with time for all the eigenmodes. This conclusion has been supported by our simulations done both on a Cartesian grid and on a curvilinear grid in spherical coordinates. Dispersion equation determining the eigenvalues of the problem and explicit formulas for the eigenfunction profiles corresponding to these eigenvalues are presented, making it possible to use the theory for hydro code verification in two and three dimensions.

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“…produced a quasi-spherical radiative blast wave, in which radiation during the shock transition is calculated to play a key role. 47 The thin, dense layers that are produced when shocked material collapses are subject to hydrodynamic instabilities like those discussed by Vishniac and Ryu. 48,49 These instabilities produce convolutions in the dense layer, observed in simulations 6,32 and believed to be responsible, for example, for the structure of the ring nebulae in WolfRayet stars.…”

Section: Radiative Shocks a Importance Of The Workmentioning

confidence: 99%

“…54 It is worth noting that the effective γ of xenon can be significantly smaller in lower-density media in (more or less) coronal equilibrium, which is the case for the experiments with blast waves in gases. 47,55 The xenon was modeled using an average-atom, LTE description, which one would expect to be only qualitatively accurate.…”

Section: B Recent Research In Radiative Shocksmentioning

confidence: 99%

Annual Report 2006 for Hydrodynamics and Radiation Hydrodynamics with Astrophysical Applications

Drake¹

2007

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Target for a supernova hydrodynamics experiment. The large acrylic shield has several advantages.Dual orthogonal backlit pinhole radiographs using ungated detectors. From experiments to study Rayleigh-Taylor evolution from a 3D sinusoidal pattern, at 21 ns. Left: an image across the CHBr strip. Right: an image down the CHBr strip. In both images dense spikes and the shockwave can be seen. They are moving to the right. The grid is for spatial calibration and magnification. The bright white feature on the left is a scratch on the film. Radiograph, of radiative shock in Xe gas after image processing to remove x-ray intensity variations.

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Dynamical Overstability of Radiative Blast Waves: The Atomic Physics of Shock Stability

Cited by 59 publications

References 37 publications

2D numerical study of the radiation influence on shock structure relevant to laboratory astrophysics

2D numerical study of the radiation influence on shock structure relevant to laboratory astrophysics

Stability of stagnation via an expanding accretion shock wave

Annual Report 2006 for Hydrodynamics and Radiation Hydrodynamics with Astrophysical Applications

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