Postcollapse hydrodynamics of SN 1987A - Two-dimensional simulations of the early evolution

Herant, Marc; Benz, W.; Colgate, Stirling A.

doi:10.1086/171685

Cited by 225 publications

(173 citation statements)

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“…Second, material advecting toward the gain surface is continually heated by neutrinos, gaining entropy as it moves inwards. As has been pointed out by many authors (e.g., Herant et al 1992Herant et al , 1994Janka & Müller 1993;Burrows et al 1995;Janka & Müller 1995;Thompson 2000;Janka 2001;Fryer & Warren 2004;Thompson et al 2005;Bruenn et al 2006;Buras et al 2006b;Murphy & Burrows 2008;Scheck et al 2008;Müller et al 2012a), convective flows enhance the conditions necessary for the revival of the shock. They increase the effective neutrino heating efficiency because rising fluid elements have lower neutrino emissivities after adiabatic expansion, reducing losses due to neutrino cooling, and the non-radial motions increase the dwell time of fluid elements in the gain region, thereby increasing the time they are subject to neutrino heating.…”

Section: Development Of Instabilities and Asphericitymentioning

confidence: 83%

“…A number of early multidimensional hydrodynamics simulations demonstrated that neutrino-driven convection does indeed develop in the heating layer and enhances the revival of the shock (Herant et al 1992(Herant et al , 1994Janka & Müller 1993Burrows et al 1995). These authors and others pointed out that convectively unstable entropy gradients occur in the heating layer for several reasons.…”

Section: Development Of Instabilities and Asphericitymentioning

confidence: 99%

“…Two decades ago, the first two-dimensional (2D) simulations (Herant et al 1992(Herant et al , 1994 transformed the field. The fundamental feedback between mass accretion, against which the shock must work, and the neutrino luminosities powering the explosion was finally unchained in these models and others (e.g., Burrows et al 1995;Janka & Müller 1996), allowing continued accretion and explosion to coexist, something impossible in 1D models.…”

Section: Introductionmentioning

confidence: 99%

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The Development of Explosions in Axisymmetric Ab Initio Core-Collapse Supernova Simulations of 12–25 Stars

Bruenn

Lentz

Hix

et al. 2016

ApJ

203

300

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We present four ab initio axisymmetric core-collapse supernova simulations initiated from 12, 15, 20, and 25 M  zero-age main sequence progenitors. All of the simulations yield explosions and havebeen evolved for at least 1.2 s after core bounce and 1 s after material first becomes unbound. These simulations were computed with our CHIMERA code employing RbR spectral neutrino transport, special and general relativistic transport effects, and state-of-the-art neutrino interactions. Continuing the evolution beyond 1 s after core bounce allows the explosions to develop more fully and the processes involved in powering the explosions to become more clearly evident. We compute explosion energy estimates, including the negative gravitational binding energy of the stellar envelope outside the expanding shock, of 0.34, 0.88, 0.38, and 0.70 Bethe (B≡10 51 erg) and increasing at 0.03, 0.15, 0.19, and 0.52 B s 1 -, respectively, for the 12, 15, 20, and 25 M  models at the endpoint of this report. We examine the growth of the explosion energy in our models through detailed analyses of the energy sources and flows. We discuss how the explosion energies may be subject to stochastic variations as exemplfied by the effect of the explosion geometry of the 20 M  model in reducing its explosion energy. We compute the proto-neutron star masses and kick velocities. We compare our results for the explosion energies and ejected Ni 56 masses against some observational standards despite the large error bars in both models and observations.

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Section: Development Of Instabilities and Asphericitymentioning

confidence: 83%

Section: Development Of Instabilities and Asphericitymentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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The Development of Explosions in Axisymmetric Ab Initio Core-Collapse Supernova Simulations of 12–25 Stars

Bruenn

Lentz

Hix

et al. 2016

ApJ

203

300

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“…This achievement was presaged by earlier studies demonstrating the tendency for convective cells to merge to the lowest order allowed by the spatial domain [45] and recognizing a new spherical accretion shock instability [46] (discovered independently in a different context in Ref. [47]).…”

Section: History Of Neutrino Radia-tion Hydrodynamicsmentioning

confidence: 96%

Supernova neutrino challenges

Cardall

2005

Nuclear Physics B - Proceedings Supplements

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A principal 'supernova neutrino challenge' is the computational difficulty of six-dimensional neutrino radiation hydrodynamics. The variety of resulting approximations has provoked a long history of uncertainty in the core-collapse supernova explosion mechanism, but recent work highlighting low-mode convection and a newlyrecognized instability in spherical accretion shocks may signal (yet another) resolution. As part of its goal of elucidating the explosion mechanism, the Terascale Supernova Initiative is committed to meeting the full complexity of the computational challenge. The understanding of supernova neutrino emission gained in detailed simulations provides a potential basis for learning about two major remaining unknowns in neutrino flavor mixing: the value of the mixing angle θ13, and distinguishing between "normal" and "inverted" mass hierarchies.

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“…In the very early phase, the high radiation pressure probably launches a second shock before the shocked material is radially accelerated as a whole. If the radiation pressure is spatially nonuniform due possibly to nonuniform neutrino heating (Burrows & Fryxell 1993 ;Keil, Janka, & 1996), then the interface between the Muller bubble and the envelope will be deformed, resulting in an "" initial ÏÏ perturbation of the subsequent Rayleigh-Taylor (R-T) instability (Chandrasekhar 1968) and convection (Herant, Benz, & Colgate 1992). The formation of the initial perturbation will end when the geometrical separation from the protoneutron star is well established or will be hidden by the R-T instability soon after the shocked material is accelerated.…”

Section: Introductionmentioning

confidence: 99%

Formation of Initial Perturbation of Rayleigh‐Taylor Instability in Supernovae and Laser‐irradiated Targets—Is There Any Similarity?

Azechi¹,

Shigemori²,

Nakai³

et al. 2000

ASTROPHYS J SUPPL S

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It is suggested that the formation of initial hydrodynamic perturbation in the early phase of supernova explosions is analogous to the initial "" imprint ÏÏ process of laser nonuniformity on a target for inertial conÐnement fusion. If the radiation pressure in supernovae is spatially nonuniform due possible to nonuniform neutrino heating, the interface between the early bubble and the envelope will be deformed, resulting in a seed of the Rayleigh-Taylor instability and convection. When laser light is Ðrst applied on a target, nonuniformity in laser irradiation is "" imprinted ÏÏ on the surface, which then set the initial perturbation of the subsequent Rayleigh-Taylor instability. We will review a reasonably simple imprint model, test it in the laser experiments, and apply it on the supernova process. If this analogy is correct, the velocity perturbation may be signiÐcantly increased compared with a secular distortion due to the pressure nonuniformity.

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Postcollapse hydrodynamics of SN 1987A - Two-dimensional simulations of the early evolution

Cited by 225 publications

References 0 publications

The Development of Explosions in Axisymmetric Ab Initio Core-Collapse Supernova Simulations of 12–25 Stars

The Development of Explosions in Axisymmetric Ab Initio Core-Collapse Supernova Simulations of 12–25 Stars

Supernova neutrino challenges

Formation of Initial Perturbation of Rayleigh‐Taylor Instability in Supernovae and Laser‐irradiated Targets—Is There Any Similarity?

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