The Hydrodynamic Behavior of Supernovae Explosions

Colgate, Stirling A.; White, Richard

doi:10.1086/148549

Cited by 910 publications

(531 citation statements)

References 1 publication

(1 reference statement)

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“…Other scenarios leading from core collapse to an explosion have been recently suggested (e.g., Wheeler et al 2000 ;Thompson 2000), but these have yet to be modeled and carefully scrutinized. The standard paradigm, which has been extensively studied for many years, is based on the original Colgate & White (1966) idea that a core collapse supernova explosion is driven by neutrino energy deposition, but the paradigm has been much modiÐed and reÐned over the intervening years. All investigators agree with the paradigmÏs account of the initial phases of the mechanism, which starts with the destabilization and collapse of the core of a massive star.…”

Section: Supernova Paradigmmentioning

confidence: 99%

General Relativistic Effects in the Core Collapse Supernova Mechanism

Bruenn

Nisco

Mezzacappa

2001

ApJ

107

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We apply our recently developed code for spherically symmetric, fully general relativistic (GR) Lagrangian hydrodynamics and multigroup Ñux-limited di †usion (MGFLD) neutrino transport to examine the e †ects of GR on the hydrodynamics and transport during collapse, bounce, and the critical shock reheating phase of core collapse supernovae. GR e †ects were examined by performing core collapse simulations from several precollapse models in the Newtonian limit, in a hybrid limit consisting of GR hydrodynamics and Newtonian transport, and in the fully GR limit. Comparisons of models computed with GR versus Newtonian hydrodynamics show that collapse to bounce takes slightly less time in the GR limit and that the shock propagates slightly farther out in radius before receding. After a secondary quasi-static rise in the shock radius, the shock radius declines considerably more rapidly in the GR simulations than in the corresponding Newtonian simulations. During the shock reheating phase, core collapse computed with GR hydrodynamics results in a substantially more compact structure from the center out to the stagnated shock, the shock radius being reduced by a factor of 2 after 300 ms for a 25 model and 600 ms for a 15 model, times being measured from bounce. The inÑow speed of M _ M _ material behind the shock is also increased by about a factor of 2 throughout most of the evolution as a consequence of GR hydrodynamics. Regarding neutrino transport, comparisons show that the luminosity and rms energy of any neutrino Ñavor during the shock reheating phase increases when switching from Newtonian to GR hydrodynamics. This arises from the close coupling of the hydrodynamics and transport and the e †ect of GR hydrodynamics to produce more compact core structures, hotter neutrinospheres at smaller radii. On additionally switching from Newtonian to GR transport, gravitational time dilation and redshift e †ects decrease the luminosities and rms energies of all neutrino Ñavors. This decrease is less in magnitude than the increase in neutrino luminosities and rms energies that arise when switching from Newtonian to GR hydrodynamics, with the result that a fully GR simulation gives higher neutrino luminosities and harder neutrino spectra than a fully Newtonian simulation of the same precollapse model.

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Section: Supernova Paradigmmentioning

confidence: 99%

General Relativistic Effects in the Core Collapse Supernova Mechanism

Bruenn

Nisco

Mezzacappa

2001

ApJ

107

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“…It has been nearly 50years since Colgate & White (1966) first proposed that core-collapse supernovae (CCSNe) may be driven by neutrino energy deposition in the mantle from neutrinos produced and transported from a gravitationally collapsing core, and most current investigations of the CCSN explosion mechanism still center around this idea. Colgate and White's seminal work was followed by increasingly sophisticated one-dimensional (1D) models that eventually included multifrequency (spectral) neutrino transport, the state of the art in weak interaction physics of the day (the impact of the newly discovered weak neutral currents was part of the important progress made through these models), a nuclear equation of state (EoS), and general relativistic treatment of gravity (Arnett 1966;Wilson 1971Wilson , 1974Bruenn 1975;Wilson et al 1975;Arnett 1977).…”

Section: Introductionmentioning

confidence: 99%

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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“…Baade and Zwicky (1934) were the first to suggest that the gravitational energy released during the formation of a neutron star could produce a supernova explosion. Colgate and White (1966) built a supernova model, considering that the transfer of energy takes place by the emission and deposition of neutrinos; Wilson (1971) showed that the electron capture neutrino burst was not strong enough to eject material. The Weinberg-Salam model of electroweak interactions opened new possibilities of neutrino interactions with matter (neutral currents).…”

Section: Thermonuclear Supernovae (Sneia)mentioning

confidence: 99%

Explosive Nucleosynthesis

Hernanz¹

2011

Encyclopedia of Astrobiology

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Many radioactive nuclei relevant for gamma-ray astrophysics are synthesized during explosive events, such as classical novae and supernovae. A review of recent results of explosive nucleosynthesis in these scenarios will be presented, with a special emphasis on the ensuing gamma-ray emission from individual nova and supernova explosions. The influence of the dynamic properties of the ejecta on the gamma-ray emission features, as well as the still remaining uncertainties in nova and supernova modelling will also be reviewed.

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The Hydrodynamic Behavior of Supernovae Explosions

Cited by 910 publications

References 1 publication

General Relativistic Effects in the Core Collapse Supernova Mechanism

General Relativistic Effects in the Core Collapse Supernova Mechanism

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

Explosive Nucleosynthesis

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