Two‐dimensional versus Three‐dimensional Supernova Hydrodynamic Instability Growth

Kane, J.; Arnett, David; Remington, B. A.; Glendinning, S. G.; Bazán, G.; Müller, Ewald; Fryxell, B.; Teyssier, Romain

doi:10.1086/308220

Cited by 73 publications

(92 citation statements)

References 25 publications

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“…This would favour a 2D simulation. However, developing turbulent structures and the occurring instabilities, which yield the break-up of the SN shell, are entirely different in 2D than in 3D (Elmegreen & Scalo 2004;Kane et al 2000). While turbulence in nature is an inherently 3D process, one might think of turbulent flows that are approximately 2D, in the sense that large scale coupling of eddies clearly exceeds the extension in one particular dimension.…”

Section: Comparison With Our Modelmentioning

confidence: 99%

3D hydrodynamic simulations of the Galactic supernova remnant CTB 109

Bolte

Sasaki

Breitschwerdt

2015

A&A

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Context. Using detailed 3D hydrodynamic simulations we study the nature of the Galactic supernova remnant (SNR) CTB 109 (G109.1-1.0), which is well known for its semicircular shape and a bright diffuse X-ray emission feature inside the SNR. Aims. Our model has been designed to explain the observed morphology, with a special emphasis on the bright emission feature inside the SNR. Moreover, we determine the age of the remnant and compare our findings with X-ray observations. With CTB 109 we test a new method of detailed numerical simulations of diffuse young objects, using realistic initial conditions derived directly from observations. Methods. We performed numerical 3D simulations with the RAMSES code. The initial density structure has been directly taken from 12 CO emission data, adding an additional dense cloud, which, when it is shocked, causes the bright emission feature.Results. From parameter studies we obtained the position ( , b) = (109.1545 • , −1.0078 • ) for an elliptical cloud with n cloud = 25 cm −3 based on the preshock density from Chandra data and a maximum diameter of 4.54 pc, whose encounter with the supernova (SN) shock wave generates the bright X-ray emission inside the SNR. The calculated age of the remnant is about 11 000 yr according to our simulations. In addition, we can also determine the most probable site of the SN explosion. Conclusions. Hydrodynamic simulations can reproduce the morphology and the observed size of the SNR CTB 109 remarkably well. Moreover, the simulations show that it is very plausible that the bright X-ray emission inside the SNR is the result of an elliptical dense cloud shocked by the SN explosion wave. We show that numerical simulations using observational data for an initial model can produce meaningful results.

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Section: Comparison With Our Modelmentioning

confidence: 99%

3D hydrodynamic simulations of the Galactic supernova remnant CTB 109

Bolte

Sasaki

Breitschwerdt

2015

A&A

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“…The simulations have either been focused on the behavior of isolated bubbles or spikes [21][22][23] or or on multimode phenomena in thin, ablative layers relevant to inertial fusion. 24 There is to our knowledge only one exploration by detailed simulations in 3D of multimode RT at an embedded interface, 25 but it is a calculation for incompressible fluids at low Re.…”

Section: Introductionmentioning

confidence: 99%

Nonlinear mixing behavior of the three-dimensional Rayleigh–Taylor instability at a decelerating interface

et al. 2004

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We report results from the first experiments to explore the evolution of the RayleighTaylor (RT) instability from intentionally three-dimensional (3D) initial conditions at an embedded, decelerating interface in a high-Reynolds-number flow. The experiments used 5 kJ of laser energy to produce a blast wave in polyimide and/or brominated plastic having an initial pressure of ~ 50 Mbars. This blast wave shocked and then decelerated the perturbed interface between first material and a lower-density, C foam. This caused the formation of a decelerating interface with an Atwood number ~2/3, producing a longterm positive growth rate for the RT instability. The initial perturbations were a 3D perturbation in an "egg-crate" pattern with feature spacings of 71 µm in two orthogonal directions and peak-to-valley amplitudes of 5 µm. The resulting RT spikes were observed to overtake the shock waves at the undisturbed, "free-fall" rate, and to subsequently deliver material from behind the interface to the forward shock. This result is unanticipated by prior simulations and models.

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“…Straightforward modeling of hydrodynamic instabilities has not produced enough mixing to explain them. 19,[58][59][60][61][62][63] Our past and planned experiments, in combination with simulations, should impact the consideration of instabilities as a potential explanation for the observations from SN1987A.…”

Section: Structure In Supernovae a Importance Of The Workmentioning

confidence: 99%

“…Spikes do experience less drag and reach higher velocities in 3D than in 2D. However, there are no 3D simulations of SN explosions, and the velocities remain too small to explain SN 1987A in 3D simulations 63,[73][74][75] and buoyancy-drag models 76,77 of isolated 3D spikes. Other existing studies of 3D RT instabilities, reviewed in Drake et al, 24 are of limited relevance for reasons discussed there.…”

Section: Structure In Supernovae a Importance Of The Workmentioning

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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Two‐dimensional versus Three‐dimensional Supernova Hydrodynamic Instability Growth

Cited by 73 publications

References 25 publications

3D hydrodynamic simulations of the Galactic supernova remnant CTB 109

3D hydrodynamic simulations of the Galactic supernova remnant CTB 109

Nonlinear mixing behavior of the three-dimensional Rayleigh–Taylor instability at a decelerating interface

Annual Report 2006 for Hydrodynamics and Radiation Hydrodynamics with Astrophysical Applications

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