The impact of vorticity waves on the shock dynamics in core-collapse supernovae

Huete, César; Abdikamalov, Ernazar; Radice, David

doi:10.1093/mnras/stx3360

Cited by 25 publications

(45 citation statements)

References 77 publications

(88 reference statements)

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“…The effect of the entropic-buoyant turbulent perturbations generated by incident vorticity waves was found to reduce the critical luminosity by ∼17-24 per cent, which approximately agrees with the results of three-dimensional simulations of CCSNe [29]. The present study is an extension of [28] and it focuses on the linear interaction of the shock with bidimensional single-mode vorticity perturbations. Employing the mathematical formalism used in describing Richtmyer-Meshkov-type flows [30,31,32] and perturbed non-reactive and reactive shocks [33,34,35,36,37,38], the exact spatial distribution of the rotational and acoustic perturbations generated in the post-shock flow are provided along with the transient evolution of the shock front towards the permanent oscillatory mode, which, akin to non-ideal gases [39,40], may change the character of the decay when nuclear dissociation is sufficiently high.…”

Section: Collapsing Starsupporting

confidence: 83%

“…The convective motion in oxygen and silicon shells may persist even during iron core collapse. As the core collapses, these shells contract and, due to the conservation of angular momentum, the velocities amplify as ∝ r −1 , resulting in an increase by a factor of several (e.g., [25,28]). Upon reaching the shock, these perturbations interact with the supernova shock and generate additional turbulence in the post-shock region.…”

Section: Collapsing Starmentioning

confidence: 99%

“…Using the linear interaction analysis (LIA), Abdikamalov et al [25,26] studied the effect of acoustic, entropy, and vorticity perturbations, which are the three components of a generic weak hydrodynamic turbulent flow [27]. Huete et al [28] improved their models by taking into account the perturbation of nuclear dissociation energy at the shock. They employed longtime asymptotic expressions to compute the turbulent amplification ratios across the shock front for incoming vorticity waves.…”

Section: Collapsing Starmentioning

confidence: 99%

“…For stalled shock in CCSNe, ∆e dis can be parametrized as ∆e dis = ευ 2 FF /2, where υ FF freefall speed and is a dimensionless parameter [42,43]. In this scenario, scales as ∼ 0.67M −1 1.3 (R shock /150 km), which results in ε typically ranging between 0.2 and 0.5 [28]. For flows with vanishing Bernoulli parameter above the shock, one can express ∆e dis in terms of the preshock Mach number M 1 = u 1 /a 1 (see [28] for the details of the derivation),…”

Section: Base-flow Equationsmentioning

confidence: 99%

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Response of nuclear-dissociating shocks to vorticity perturbations

Huete

Abdikamalov

2019

Phys. Scr.

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In the context of core-collapse supernova explosions (CCSNe), the interaction of standing accretion shocks with upstream vorticity perturbations is investigated by linear theory analysis. The endothermic effect associated to the nuclear dissociation, which takes place right behind the shock wave, affects the amplitude of the perturbations amplified/generated across the front. For upstream disturbances whose characteristic size is much larger than the post-shock dissociationlayer thickness, the effect of nuclear dissociation can be reduced to that of considering the global endothermic effect that scales with the inflow energy flux. The present study focuses on perturbation fields that are not isotropic, which mimic the perturbations in collapsing convective shells of massive stars. The linear interaction of the shock with bidimensional mono-frequency vorticity perturbations is theoretically addressed, with the limit of highly-stretched vortices being analyzed in detail. The exact spatial distribution of the rotational and acoustic perturbations generated in the post-shock flow are provided along with the transient evolution of the shock front. It is found that nuclear dissociation contributes to stabilize the shock oscillations, but increases the amplitude of the density perturbations downstream. An extension of this work that addresses the interaction with tridimensional isotropic turbulent flows can be found in reference Huete, C., et al. 2018, MNRAS, 475, 33053323, which analyzes the effect of the post-shock flow on the critical conditions that ultimately trigger explosion.

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Section: Collapsing Starsupporting

confidence: 83%

Section: Collapsing Starmentioning

confidence: 99%

Section: Collapsing Starmentioning

confidence: 99%

Section: Base-flow Equationsmentioning

confidence: 99%

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Response of nuclear-dissociating shocks to vorticity perturbations

Huete

Abdikamalov

2019

Phys. Scr.

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“…In addition, the convective eddies have to constantly adjust to new pressure equilibriums, a process that generates strong acoustic waves (e.g., Foglizzo & Tagger 2000). When these perturbations arrive ahead of the supernova shock, their physical properties affect they way they interact with the shock (Abdikamalov et al 2016;Abdikamalov et al 2018;Huete et al 2018;Huete & Abdikamalov 2019;Radice et al 2018).…”

Section: Introductionmentioning

confidence: 99%

Acoustic wave generation in collapsing massive stars with convective shells

Abdikamalov

Foglizzo

2020

Monthly Notices of the Royal Astronomical Society

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The convection that takes place in the innermost shells of massive stars plays an important role in the formation of core-collapse supernova explosions. Upon encountering the supernova shock, additional turbulence is generated, amplifying the explosion. In this work, we study how the convective perturbations evolve during the stellar collapse. Our main aim is to establish their physical properties right before they reach the supernova shock. To this end, we solve the linearized hydrodynamics equations perturbed on a stationary background flow. The latter is given by the spherical transonic Bondi accretion, while the convective perturbations are modeled as a combination of entropy and vorticity waves. We follow their evolution from large radii, where convective shells are initially located, down to small radii, where they are expected to encounter the accretion shock above the proto-neutron star. Considering typical vorticity perturbations with a Mach number ∼ 0.1 and entropy perturbations δS ∼ 0.05k b /baryon at a radius of 1, 500 km, we find that the advection of these perturbations down to the shock generates strong acoustic waves with a relative amplitude δp/γp ∼ 10%, in agreement with numerical simulations. The velocity perturbations consist of comparable contributions from vorticity and acoustic waves with values reaching 10% of the sound speed ahead of the shock.

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Hydrodynamics of core-collapse supernovae and their progenitors

Müller¹

2020

Living Rev Comput Astrophys

146

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Multi-dimensional fluid flow plays a paramount role in the explosions of massive stars as core-collapse supernovae. In recent years, three-dimensional (3D) simulations of these phenomena have matured significantly. Considerable progress has been made towards identifying the ingredients for shock revival by the neutrino-driven mechanism, and successful explosions have already been obtained in a number of selfconsistent 3D models. These advances also bring new challenges, however. Prompted by a need for increased physical realism and meaningful model validation, supernova theory is now moving towards a more integrated view that connects multi-dimensional phenomena in the late convective burning stages prior to collapse, the explosion engine, and mixing instabilities in the supernova envelope. Here we review our current understanding of multi-D fluid flow in core-collapse supernovae and their progenitors. We start by outlining specific challenges faced by hydrodynamic simulations of core-collapse supernovae and of the late convective burning stages. We then discuss recent advances and open questions in theory and simulations.

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The impact of vorticity waves on the shock dynamics in core-collapse supernovae

Cited by 25 publications

References 77 publications

Response of nuclear-dissociating shocks to vorticity perturbations

Response of nuclear-dissociating shocks to vorticity perturbations

Acoustic wave generation in collapsing massive stars with convective shells

Hydrodynamics of core-collapse supernovae and their progenitors

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