Scattering functions for neutrino transport

Yueh, William R.; Buchler, J. R.

doi:10.1007/bf00648341

Cited by 34 publications

(31 citation statements)

References 2 publications

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“…The neutrino pair-emissivity from electron-positron annihilation was calculated by Yueh & Buchler (1976a) and Yueh & Buchler (1976b). They explored the possibility of calculating the pairreaction rates in a similar way as neutrino-electron scattering (NES).…”

Section: Appendixmentioning

confidence: 99%

The neutrino signal from protoneutron star accretion and black hole formation

Fischer

Whitehouse

Mezzacappa

et al. 2009

A&A

193

180

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Context. We discuss the formation of stellar mass black holes via protoneutron star (PNS) collapse. In the absence of an earlier explosion, the PNS collapses to a black hole due to the continued mass accretion onto the PNS. We present an analysis of the emitted neutrino spectra of all three flavors during the PNS contraction. Aims. Special attention is given to the physical conditions which depend on the input physics, e.g. the equation of state (EoS) and the progenitor model. Methods. The PNSs are modeled as the central object in core collapse simulations using general relativistic three-flavor Boltzmann neutrino transport in spherical symmetry. The simulations are launched from several massive progenitors of 40 M and 50 M . Results. We analyze the electron-neutrino luminosity dependencies and construct a simple approximation for the electron-neutrino luminosity, which depends only on the physical conditions at the electron-neutrinosphere. In addition, we analyze different (μ, τ)-neutrino pair-reactions separately and compare the differences during the post-bounce phases of failed core collapse supernova explosions of massive progenitors. We also investigate the connection between the increasing (μ, τ)-neutrino luminosity and the PNS contraction during the accretion phase before black hole formation. Conclusions. Comparing the different post bounce phases of the progenitor models under investigation, we find large differences in the emitted neutrino spectra. These differences and the analysis of the electron-neutrino luminosity indicate a strong progenitor model dependency of the emitted neutrino signal.

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Section: Appendixmentioning

confidence: 99%

The neutrino signal from protoneutron star accretion and black hole formation

Fischer

Whitehouse

Mezzacappa

et al. 2009

A&A

193

180

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“…Fortunately, we were lucky to express moments of the neutrino spectrum by the Fermi-Dirac integrals (21). With the moments given, one is able to approximate the spectrum with the aid of an appropriate analytical formula.…”

Section: Neutrino Energy Momentsmentioning

confidence: 99%

Neutrino spectrum from the pair-annihilation process in the hot stellar plasma

2006

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An new method of calculating the energy spectrum of neutrinos and antineutrinos produced in the electron-positron annihilation processes in hot stellar plasma is presented. Detection of these neutrinos, produced copiously in the presupernova which is evolutionary advanced neutrino-cooled star, may serve in future as a trigger of pre-collapse early warning system. Also, observation of neutrinos will probe final stages of thermonuclear burning in the presupernova.The spectra obtained with the new method are compared to Monte Carlo simulations. To achieve high accuracy in the energy range of interest, determined by neutrino detector thresholds, differential cross-section for production of the antineutrino, previously unknown in an explicit form, is calculated as a function of energy in the plasma rest frame. Neutrino spectrum is obtained as a 3-dimensional integral, computed with the use of the Cuhre algorithm of at least 5% accuracy. Formulae for the mean neutrino energy and its dispersion are given as a combination of Fermi-Dirac integrals. Also, useful analytical approximations of the whole spectrum are shown.

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“…Finally, the neutrino interactions with matter used for supernova simulations have been computed assuming that neutrinos interact with an isolated nucleons (e.g., Freedman 1974 ;Tubbs & Schramm 1975 ;Yueh & Buchler 1976a, 1976b, 1977Bruenn 1985). Nucleon blocking and spatial correlations have been inadequately incorporated, and nucleon thermal motions, recoil, and temporal correlations have been ignored.…”

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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Scattering functions for neutrino transport

Cited by 34 publications

References 2 publications

The neutrino signal from protoneutron star accretion and black hole formation

The neutrino signal from protoneutron star accretion and black hole formation

Neutrino spectrum from the pair-annihilation process in the hot stellar plasma

General Relativistic Effects in the Core Collapse Supernova Mechanism

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