Turbulence Generation by Shock-Acoustic-Wave Interaction in Core-Collapse Supernovae

Abdikamalov, Ernazar; Huete, César; Nussupbekov, Ayan; Berdibek, Shapagat

doi:10.48550/arxiv.1805.03957

Cited by 2 publications

(3 citation statements)

References 39 publications

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“…However, the analysis of Müller et al (2016b) did not account in detail for the interaction of the infalling perturbations with the shock. This has been investigated using linear perturbation theory (Takahashi et al 2016;Abdikamalov et al 2016Abdikamalov et al , 2018Huete et al 2018;Huete and Abdikamalov 2019). As a downside, this perturbative approach cannot easily capture the non-linear interaction of the injected perturbations with fully developed neutrino-driven convection and the SASI, but Huete et al (2018) recently incorporated the effects of buoyancy downstream of the shock.…”

Section: Perturbation-aided Explosionsmentioning

confidence: 99%

Hydrodynamics of core-collapse supernovae and their progenitors

Müller

2020

Preprint

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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 neutrinodriven mechanism, and successful explosions have already been obtained in a number of self-consistent 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 multidimensional 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 understasnding 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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Section: Perturbation-aided Explosionsmentioning

confidence: 99%

Hydrodynamics of core-collapse supernovae and their progenitors

Müller

2020

Preprint

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“…The interaction of outgoing acoustic waves with the stalled shock has been studied extensively in the context of the SASI (see, e.g., Foglizzo et al 2007;Foglizzo 2009;Guilet et al 2010;Guilet & Foglizzo 2012), but the particulars of the wave-shock interaction are beyond the scope of this study and left to future work. We also direct the interested reader to work by Abdikamalov et al (2016); Huete et al (2018); Abdikamalov et al (2018) for discussions on the interaction of waves with the stalled shock.…”

Section: Impact Of Waves On Shock Revivalmentioning

confidence: 99%

“…While failed explosions are still seen with these more involved simulations, several studies have shown that the evolutionary track for many models exists near the boundary between successful explosion and failed supernova. It has been shown that modest changes to input physics and numerical techniques such as, for example, using more realistic input data for the progenitor models, can reduce the critical neutrino luminosity required for a successful explosion to develop Abdikamalov et al 2016Abdikamalov et al , 2018.…”

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confidence: 99%

Wave heating from proto-neutron star convection and the core-collapse supernova explosion mechanism

Gossan

Fuller

Roberts

2019

Monthly Notices of the Royal Astronomical Society

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Our understanding of the core-collapse supernova explosion mechanism is incomplete. While the favoured scenario is delayed revival of the stalled shock by neutrino heating, it is difficult to reliably compute explosion outcomes and energies, which depend sensitively on the complex radiation hydrodynamics of the post-shock region. The dynamics of the (non-)explosion depend sensitively on how energy is transported from inside and near the proto-neutron star (PNS) to material just behind the supernova shock. Although most of the PNS energy is lost in the form of neutrinos, hydrodynamic and hydromagnetic waves can also carry energy from the PNS to the shock. We show that gravity waves excited by core PNS convection can couple with outgoing acoustic waves that present an appreciable source of energy and pressure in the post-shock region. Using one-dimensional simulations, we estimate the gravity wave energy flux excited by PNS convection and the fraction of this energy transmitted upward to the post-shock region as acoustic waves. We find wave energy fluxes near 10 51 erg s −1 are likely to persist for ∼ 1 s post-bounce. The wave pressure on the shock may exceed 10% of the thermal pressure, potentially contributing to shock revival and, subsequently, a successful and energetic explosion. We also discuss how future simulations can better capture the effects of waves, and more accurately quantify wave heating rates.

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Turbulence Generation by Shock-Acoustic-Wave Interaction in Core-Collapse Supernovae

Cited by 2 publications

References 39 publications

Hydrodynamics of core-collapse supernovae and their progenitors

Hydrodynamics of core-collapse supernovae and their progenitors

Wave heating from proto-neutron star convection and the core-collapse supernova explosion mechanism

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