Simulation of the growth of the 3D Rayleigh-Taylor instability in supernova remnants using an expanding reference frame

Fraschetti, Federico; Teyssier, Romain; Ballet, J.; Decourchelle, A.

doi:10.1051/0004-6361/200912692

Cited by 41 publications

(46 citation statements)

References 52 publications

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“…We detail here the transformation that makes the computational grid co-expand with the SNR, without any need to add grid cells or refinement layers. The technique is commonly used for cosmological simulations, it was applied to SNRs by Fraschetti et al (2010), following Poludnenko & Khokhlov (2007). 9 Everywhere in this section tilde quantities refer to transformed quantities, i.e.…”

Section: Resultsmentioning

confidence: 99%

From Supernova to Supernova Remnant: The Three-dimensional Imprint of a Thermonuclear Explosion

Ferrand

Warren

Ono

et al. 2019

ApJ

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Recent progress in the three-dimensional modeling of supernovae (SN) has shown the importance of asymmetries for the explosion. This calls for a reconsideration of the modeling of the subsequent phase, the supernova remnant (SNR), which has commonly relied on simplified ejecta models. In this paper we bridge SN and SNR studies by using the output of a SN simulation as the input of a SNR simulation carried on until 500 yr. We consider the case of a thermonuclear explosion of a carbonoxygen white dwarf star as a model for a Type Ia SN; specifically we use the N100 delayed detonation model of Seitenzahl et al 2013. In order to analyze the morphology of the SNR, we locate the three discontinuities that delineate the shell of shocked matter: the forward shock, the contact discontinuity, and the reverse shock, and we decompose their radial variations as a function of angular scale and time. Assuming a uniform ambient medium, we find that the impact of the SN on the SNR may still be visible after hundreds of years. Previous 3D simulations aiming at reproducing Tycho's SNR, that started out from spherically symmetric initial conditions, failed to reproduce structures at the largest angular scales observed in X-rays. Our new simulations strongly suggest that the missing ingredient was the initial asymmetries from the SN itself. With this work we establish a way of assessing the viability of SN models based on the resulting morphology of the SNR.

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Section: Resultsmentioning

confidence: 99%

From Supernova to Supernova Remnant: The Three-dimensional Imprint of a Thermonuclear Explosion

Ferrand

Warren

Ono

et al. 2019

ApJ

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“…Magnetic field may also be enhanced by field line stretching due to Rayleigh-Taylor (RT) instability (Jun et al 1995) at the interface between the ejecta and the interstellar medium, i.e., far downstream of the shock. In contrast with the vortical turbulence, late-time RT turbulence might be affected by the highest energy particle gyrating in the downstream fluid far from the shock (Fraschetti et al 2010). However, RT structures are unlikely to reach out the blast wave ( (Fraschetti et al 2010) and references therein) and therefore to interact with vortical turbulence.…”

Section: Introductionmentioning

confidence: 99%

“…In contrast with the vortical turbulence, late-time RT turbulence might be affected by the highest energy particle gyrating in the downstream fluid far from the shock (Fraschetti et al 2010). However, RT structures are unlikely to reach out the blast wave ( (Fraschetti et al 2010) and references therein) and therefore to interact with vortical turbulence. Thus the dynamo amplification local behind the shock can be temporally and spatially disentangled from the field line stretching due to RT instability.…”

Section: Introductionmentioning

confidence: 99%

Turbulent Amplification of a Magnetic Field Driven by the Dynamo Effect at Rippled Shocks

Fraschetti

2013

ApJ

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We derive analytically the vorticity generated downstream of a two-dimensional rippled hydromagnetic shock neglecting fluid viscosity and resistivity. The growth of the turbulent component of the downstream magnetic field is driven by the vortical eddies motion. We determine an analytic time-evolution of the magnetic field amplification at shocks, so far described only numerically, until saturation occurs due to seed-field reaction to field lines whirling. The explicit expression of the amplification growth rate and of the non-linear field back-reaction in terms of the parameters of shock and interstellar density fluctuations is derived from MHD jump conditions at rippled shocks. A magnetic field saturation up to the order of milligauss and a short-time variability in the X-ray observations of supernova remnants can be obtained by using reasonable parameters for the interstellar turbulence.

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“…Figure 1 shows the 3D rendering of the mass density at t = 1000 yr in the three cases of γ considered for uniform ISMF. The main effect of γ on the shock dynamics is to change its compression ratio and the distance of the contact discontinuity from the blast wave position (see also Fraschetti et al 2010, for the effects of accelerated CRs on the development of the Rayleigh-Taylor structures); no dependence on the obliquity angle is present, γ being uniform in each simulation. The value of γ is expected therefore to influence the absolute values of emission in the radio, X-ray, and γ-ray bands but not the large-scale morphology of the remnant to which this paper is focused on.…”

Section: Synchrotron and Ic Images Of Snrs Expanding Through A Non-unmentioning

confidence: 99%

Effects of non-uniform interstellar magnetic field on synchrotron X-ray and inverse-Comptonγ-ray morphology of supernova remnants

Orlando

Petruk

Bocchino

et al. 2011

A&A

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Context. Observations of SuperNova Remnants (SNRs) in X-ray and γ-ray bands promise to contribute important information to our understanding of the kinematics of charged particles and magnetic fields in the vicinity of strong non-relativistic shocks and, therefore, the nature of Galactic cosmic rays. The accurate analysis of SNR images collected in different energy bands requires theoretical modeling of synchrotron and inverse Compton emission from SNRs. Aims. We develop a numerical code (remlight) to synthesize, from MHD simulations, the synchrotron radio, X-ray, and inverse Compton γ-ray emission originating in SNRs expanding in a non-uniform interstellar medium (ISM) and/or non-uniform interstellar magnetic field (ISMF). As a first application, the code is used to investigate the effects of non-uniform ISMF on the SNR morphology in the non-thermal X-ray and γ-ray bands. Methods. We perform 3D MHD simulations of a spherical SNR shock expanding through a magnetized ISM with a gradient of ambient magnetic field strength. The model includes an approximate treatment of upstream magnetic field amplification and the effect of shock modification due to the back reaction of accelerated cosmic rays, assuming both effects to be isotropic. From the simulations, we synthesize the synchrotron radio, X-ray, and inverse Compton γ-ray emission with the synthesis code remlight, making different assumptions about the details of acceleration and the injection of relativistic electrons. Results. A gradient in the ambient magnetic field strength induces asymmetric morphologies in radio, hard X-ray, and γ-ray bands independently of the model of electron injection if the gradient has a component perpendicular to the line-of-sight (LoS). The degree of asymmetry of the remnant morphology depends on the details of the electron injection and acceleration and is different in the radio, hard X-ray, and γ-ray bands. In general, the non-thermal X-ray morphology is the most sensitive to the gradient, showing the highest degree of asymmetry. The IC γ-ray emission is weakly sensitive to the non-uniform ISMF, the degree of asymmetry of the remnant morphology being the lowest in this band.

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Simulation of the growth of the 3D Rayleigh-Taylor instability in supernova remnants using an expanding reference frame

Cited by 41 publications

References 52 publications

From Supernova to Supernova Remnant: The Three-dimensional Imprint of a Thermonuclear Explosion

From Supernova to Supernova Remnant: The Three-dimensional Imprint of a Thermonuclear Explosion

Turbulent Amplification of a Magnetic Field Driven by the Dynamo Effect at Rippled Shocks

Effects of non-uniform interstellar magnetic field on synchrotron X-ray and inverse-Comptonγ-ray morphology of supernova remnants

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