Similarity Criteria for the Laboratory Simulation of Supernova Hydrodynamics

Ryutov, D. D.; Drake, R. P.; Kane, J.; Liang, Edison; Remington, B. A.; Wood‐Vasey, W. M.

doi:10.1086/307293

Cited by 417 publications

(376 citation statements)

References 32 publications

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“…A fluid description should be appropriate for the plasma, and restrictions on the Reynolds, and Peclet numbers ensure that the energy flow is dominated by heat convection, while dissipative effects such as viscosity, and thermal conductivity are negligible as concluded by Ryutov et al (1999). For the jets to be collisional we require that the ion mean free path be less then the radius of the jets.…”

Section: Estimation Of Dimensionless Scaling Parametersmentioning

confidence: 99%

“…Recently, there has been particular interest in laboratory produced supersonic plasma jets because of their potential similarities to astrophysical phenomena as investigated by Ryutov et al (1999) and in further detail by Ryutov et al (2000). To model such objects in the laboratory, Lebedev et al (2002, and Ampleford et al (2008) used conical wire arrays to produce highly collimated, radiative cooled jets.…”

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confidence: 99%

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Supersonic jet formation and propagation in x-pinches

Haas

Bott

Kim

et al. 2011

Astrophys Space Sci

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Observations of supersonic jet propagation in low-current x-pinches are reported. X-pinches comprising of four 7.5 µm diameter tungsten wires were driven by an 80 kA, 50 ns current pulse from a compact pulser. Coronal plasma surrounding the wire cores was accelerated perpendicular to their surface due to the global J × B force, and traveled toward the axis of the x-pinch to form an axially propagating jet. These jets moved towards the electrodes and, late in time (∼150 ns), were observed to propagate well above the anode with a velocity of 3.3 ± 0.6 × 10 4 m/s. Tungsten jets remained collimated at distances of up to 16 mm from the cross point, and an estimate of the local sound speed gives a Mach number of ∼6. This is the first demonstration that supersonic plasma jets can be produced using x-pinches with such a small, low current pulser. Experimental data compares well to three-dimensional simulations using the GORGON resistive MHD code, and possible scaling to astrophysical jets is discussed.

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Section: Estimation Of Dimensionless Scaling Parametersmentioning

confidence: 99%

mentioning

confidence: 99%

Supersonic jet formation and propagation in x-pinches

Haas

Bott

Kim

et al. 2011

Astrophys Space Sci

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“…In situ magnetic field measurements are made in the turbulent wake of the shock. Using hydrodynamic scaling relations 17,18 , our experimental conditions at 0.3 µs after the laser illumination can be scaled to Cassiopeia A signal to noise (SNR) with a probable age t SNR of approximately 310 years, an expansion velocity v SNR of about 4,700 km s −1 and a deceleration parameter v SNR t SNR /R SNR , where R SNR is the shock radius, of about 0.6 (ref . 2; see Supplementary Information for the description of the scaling relations, and Supplementary Table 1).…”

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confidence: 99%

Turbulent amplification of magnetic fields in laboratory laser-produced shock waves

et al. 2014

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X-ray 1-3 and radio 4-6 observations of the supernova remnant Cassiopeia A reveal the presence of magnetic fields about 100 times stronger than those in the surrounding interstellar medium. Field coincident with the outer shock probably arises through a nonlinear feedback process involving cosmic rays 2,7,8 . The origin of the large magnetic field in the interior of the remnant is less clear but it is presumably stretched and amplified by turbulent motions. Turbulence may be generated by hydrodynamic instability at the contact discontinuity between the supernova ejecta and the circumstellar gas 9 . However, optical observations of Cassiopeia A indicate that the ejecta are interacting with a highly inhomogeneous, dense circumstellar cloud bank formed before the supernova explosion 10-12 . Here we investigate the possibility that turbulent amplification is induced when the outer shock overtakes dense clumps in the ambient medium 13-15 . We report laboratory experiments that indicate the magnetic field is amplified when the shock interacts with a plastic grid. We show that our experimental results can explain the observed synchrotron emission in the interior of the remnant. The experiment also provides a laboratory example of magnetic field amplification by turbulence in plasmas, a physical process thought to occur in many astrophysical phenomena.High-resolution X-ray images and radio polarization maps of Cassiopeia A show two distinct strong magnetic field regions [3][4][5][6]12 . Narrow X-ray filaments, a fraction of a parsec in width, are observed at the outer shock rim at a radius of about 2.5 pc. These structures are produced by synchrotron radiation from ultrarelativistic electrons (with teraelectronvolt energy) and can be explained by magnetic fields of the order of 100 µG or more 2,3 . The interior of the remnant contains a disordered shell (about 0.5 pc in width at a radius of 1.7 pc) of radio synchrotron emission by gigaelectronvolt electrons 4 . The inferred magnetic field in these radio knots is a few milligauss, about 100 times higher than expected from the standard shock compression of the interstellar medium 15 . Optical observations of Cassiopeia A show the presence of both rapidly moving (5,000-9,000 km s −1 ) and essentially stationary dense knots. Although the moving knots themselves have a high velocity, their overall pattern is nearly stationary 10 . This led to the suggestion 10 that a dense pre-existing inhomogeneous stationary cloud bank could be present. New rapidly moving knots predominantly appear at a position broadly coincident with the shell of bright radio emission 6 . Sizes of the observed small-scale features within the shell range from 0.01 to 0.1 pc arranged in larger patterns extending to 0.5-2 pc (ref. 16). Interaction between the ejecta and the cloud bank may excite the turbulence that amplifies the magnetic field and makes Cassiopeia A an exceptionally bright radio source 4 . The interaction is akin to the Rayleigh-Taylor instability otherwise proposed as a source of turbulenc...

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“…Whether the experiment is well scaled with regard to this physical mechanism is not clear. It may not be, because the compression produced by radiative collapse is much larger in astrophysical systems than in laboratory ones [Ryutov et al, 1998]. …”

Section: Thus the Experiments Confirmed The Central Results Of The Theorymentioning

confidence: 99%

Laboratory experiments to simulate the hydrodynamics of supernova remnants and supernovae

Drake¹

1999

J. Geophys. Res.

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Abstract. Recent years have seen the emergence of a new approach to the laboratory simulation of astrophysical phenomena. Current experiments are designed to address, with good dimensionless scaling, specific physical issues that matter to the astrophysics. These include experiments to address the hydrodynamic evolution and instabilities in supernova remnants, experiments to address hydrodynamic instabilities in core-collapse supernova explosions, and experiments to address the structure of thermonuclear supernova explosions. They are contrasted with somewhat older experiments that made first attempts in this direction, examining high-velocity spherical expansions into unmagnetized plasma, and the deceleration of spherical expansions by a magnetic field. IntroductionIn recent decades, improved instrumentation has opened our eyes to the incredible structure present in extraterrestrial space. In the realm of supernova remnants (SNRs), we have seen that these are highly structured objects. All of this poses severe challenges for theoretical modeling aimed at understanding these systems. Rather than using onedimensional models, into which one might hope to include a great deal of physics, researchers are forced to use two-and In this context, laboratory experiments have a real role to play. They can address specific issues in the development of structure in SNRs and SNe. In some cases, they can be good physical models of the actual dynamics, as is discussed in section 2. Even when they are not, they can provide real tests of the complicated computational models used to analyze the astrophysical phenomena. Several such experiments now exist, and the present paper reviews this work. The author would argue that such research can make an important contribution, both through direct simulation that tests our understanding of the underlying physics and through performing well-defined experiments that test computational models. This is needed, since building any computational model involves some compromise in the detailed physics and introduces factor such as numerical viscosity and numerical diffusion that are not present in the actual system. However, such experiments can never be extensive or versatile enough to replace computational models in the quest to understand astrophysical dynam-

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Similarity Criteria for the Laboratory Simulation of Supernova Hydrodynamics

Cited by 417 publications

References 32 publications

Supersonic jet formation and propagation in x-pinches

Supersonic jet formation and propagation in x-pinches

Turbulent amplification of magnetic fields in laboratory laser-produced shock waves

Laboratory experiments to simulate the hydrodynamics of supernova remnants and supernovae

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