Deflagration-to-detonation transition by amplification of acoustic waves in type Ia supernovae

Charignon, Camille; Chièze, J. P.

doi:10.1051/0004-6361/201220483

Cited by 10 publications

(10 citation statements)

References 27 publications

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“…To trigger the DDT, the Zel'dovich gradient mechanism (Zel'dovich et al 1972) is used. Besides, there are also other proposed mechanisms (Charignon & Chièze 2013). In the Zel'dovich mechanism, the local eddy motions near the flame front would help flatten the temperature gradient to trigger the DDT.…”

Section: Dm-admixed Thermonuclear Supernovaementioning

confidence: 99%

Delayed Detonation Thermonuclear Supernovae with an Extended Dark Matter Component

Chan

Chu

Leung

et al. 2021

ApJ

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We present spherically symmetric simulations of the thermonuclear explosion of a white dwarf admixed with an extended component of fermionic dark matter, using the deflagration model with the deflagration-detonation transition. In all the dark matter admixed models we have considered, the dark matter is left behind after the explosion as a compact dark star. The presence of dark matter lengthens the deflagration phase to produce a similar amount of iron-group elements and more thermoneutrinos. Dark matter admixed models also give dimmer but slowly declining light curves, consistent with some observed peculiar supernovae. Our results suggest a formation path for dark compact objects that mimic sub-solar-mass black holes as dark gravitational sources.Unified Astronomy Thesaurus concepts: Dark matter (353); Type Ia supernovae (1728); Hydrodynamical simulations (767); Supernova neutrinos (1666); Light curves (918) The Deflagration-Detonation Transition (DDT) as a Supernova Explosion ModelWDs are believed to be the progenitors for thermonuclear supernovae (Hillebrandt et al. 2013;Maoz et al. 2014;Livio & Mazzali 2018). However, it is not clear which kind of WDs and explosion mechanisms are responsible for such energetic events (Ruiter 2019). It is believed that most of the progenitor

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Section: Dm-admixed Thermonuclear Supernovaementioning

confidence: 99%

Delayed Detonation Thermonuclear Supernovae with an Extended Dark Matter Component

Chan

Chu

Leung

et al. 2021

ApJ

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“…And, our result holds equally well for planar, cylindrical, or spherical symmetry, and for inward as well as outward propagation. Shock formation is used in fields as diverse as the heating of the Solar corona (Osterbrock 1961), the deflagration-to-detonation transition in type Ia supernovae (Charignon & Chièze 2013), and sonoluminescence (LS01), among others, so this general result should be widely applicable.…”

Section: Detailed Derivation Of Shock Formation Radiusmentioning

confidence: 99%

Shock Dynamics in Stellar Outbursts. I. Shock Formation

Matzner

2017

ApJ

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Wave-driven outflows and non-disruptive explosions have been implicated in pre-supernova outbursts, supernova impostors, LBV eruptions, and some narrow-line and superluminous supernovae. To model these events, we investigate the dynamics of stars set in motion by strong acoustic pulses and wave trains, focusing here on nonlinear wave propagation, shock formation, and an early phase of the development of a weak shock. We identify the shock formation radius, showing that a heuristic estimate based on crossing characteristics matches an exact expansion around the wave front and verifying both with numerical experiments. Our general analytical condition for shock formation applies to one-dimensional motions within any static environment, including both eruptions and implosions, and can easily be extended to non-stationary flows. We also consider the early phase of shock energy dissipation. We find that waves of super-Eddington acoustic luminosity always create shocks, rather than damping by radiative diffusion. Therefore, shock formation is integral to super-Eddington outbursts.

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“…where f stands for the wave frequency (Ulmschneider 1970;Charignon & Chièze 2013). The derivation of that expression is presented in appendix B.…”

Section: Wave Dissipation In the Dead-zonementioning

confidence: 99%

Thermodynamics of the dead-zone inner edge in protoplanetary disks

Faure

Fromang

Latter

2014

A&A

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Context. In protoplanetary disks, the inner boundary between the turbulent and laminar regions could be a promising site for planet formation, thanks to the trapping of solids at the boundary itself or in vortices generated by the Rossby wave instability. At the interface, the disk thermodynamics and the turbulent dynamics are entwined because of the importance of turbulent dissipation and thermal ionization. Numerical models of the boundary, however, have neglected the thermodynamics, and thus miss a part of the physics. Aims. The aim of this paper is to numerically investigate the interplay between thermodynamics and dynamics in the inner regions of protoplanetary disks by properly accounting for turbulent heating and the dependence of the resistivity on the local temperature. Methods. Using the Godunov code RAMSES, we performed a series of 3D global numerical simulations of protoplanetary disks in the cylindrical limit, including turbulent heating and a simple prescription for radiative cooling. Results. We find that waves excited by the turbulence significantly heat the dead zone, and we subsequently provide a simple theoretical framework for estimating the wave heating and consequent temperature profile. In addition, our simulations reveal that the dead-zone inner edge can propagate outward into the dead zone, before stalling at a critical radius that can be estimated from a meanfield model. The engine driving the propagation is in fact density wave heating close to the interface. A pressure maximum appears at the interface in all simulations, and we note the emergence of the Rossby wave instability in simulations with extended azimuth. Conclusions. Our simulations illustrate the complex interplay between thermodynamics and turbulent dynamics in the inner regions of protoplanetary disks. They also reveal how important activity at the dead-zone interface can be for the dead-zone thermodynamic structure.

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Deflagration-to-detonation transition by amplification of acoustic waves in type Ia supernovae

Cited by 10 publications

References 27 publications

Delayed Detonation Thermonuclear Supernovae with an Extended Dark Matter Component

Delayed Detonation Thermonuclear Supernovae with an Extended Dark Matter Component

Shock Dynamics in Stellar Outbursts. I. Shock Formation

Thermodynamics of the dead-zone inner edge in protoplanetary disks

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