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Neutrino Opacities in Nuclear Matter
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Neutrino-matter cross sections and interaction rates are central to the core-collapse supernova phenomenon and, very likely, to the viability of the explosion mechanism itself. In this paper, we describe the major neutrino scattering, absorption, and production processes that together influence the outcome of core collapse and the cooling of protoneutron stars. One focus is on energy redistribution and many-body physics, but our major goal is to provide a useful resource for those interested in supernova neutrino microphysics.
Forward citations
Cited by 9 Pith papers
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The Gravitational-Wave Power Gap in Core-Collapse Supernovae: Insights from 60 Axisymmetric Simulations
The gravitational-wave power-gap frequency in core-collapse supernova simulations correlates with inner protoneutron-star properties and may arise from Fano-type interference.
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On the difficulty of capturing the distribution function of neutrinos in neutron star merger simulations
Monte Carlo merger simulations need about a thousand packets per energy and angular bin, nonstandard packet weighting, and spatial smoothing before they can estimate the neutrino distribution function to an absolute a...
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Neutrino flavor instabilities in a binary neutron star merger remnant: Roles of a long-lived hypermassive neutron star
In a long-lived hypermassive neutron star merger remnant, fast flavor instabilities occur transiently and locally while collisional flavor instabilities persist widely in the disk for about one second.
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Open-source library for performance-portable neutrino reaction rates: Application to neutron star mergers
A new open-source neutrino-rate library shows that inelastic neutrino-electron/positron scattering and nucleon decay reactions materially change neutrino opacities and decoupling surfaces in neutron star merger conditions.
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Thermodynamics conditions of matter in the neutrino decoupling region during neutron star mergers
In neutron star merger remnants, neutrinos decouple at densities around 10^11 g/cm^3 for average energies, while heavy-flavor neutrinos freeze out of equilibrium deeper, at several times 10^12 g/cm^3.
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Unequal Mass Binary Neutron Star Simulations with Neutrino Transport: Ejecta and Neutrino Emission
New simulations of unequal-mass neutron star mergers find that only the softest equation of state ejects more than 0.01 solar masses of dynamical ejecta, and that ejecta speed and electron fraction drop as the mass ra...
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Assessing the Relative Importance of Neutrino Matter Interaction Channels in Post-Merger Remnant of Binary Neutron Stars
Monte Carlo simulation of post-merger remnant shows pair annihilation rates greatly increased in cold low-density regions and inelastic electron scattering important for heavy-lepton neutrino thermalization, processes...
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Influence of neutrino-electron scattering and neutrino-pair annihilation on hypermassive neutron star
Inelastic neutrino-electron scattering in hypermassive neutron star simulations increases disc mass by 75% and ejecta mass by 18% with higher neutrino luminosities, while electron-positron annihilation shows no signif...
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Neutrinos from explosive transients at the dawn of multi-messenger astronomy
This review summarizes the state of neutrino emission from supernovae and neutron-star mergers, covering thermal and high-energy signals, flavor conversion, and multi-messenger detection strategies.
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