Neutrino opacities in nuclear matter

By Adam Burrows, S. Reddy, T. Thompson. 2004

202 citations recorded by the source corpus.

Abstract 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.

Subfields: Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/b5db79fcfb2b5d7d9f8e8921f68fe024a0e2d67a

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In Nuclear and High Energy Physics

Citations in the corpus

Mass Ejection from the Remnant of a Binary Neutron Star Merger: Viscous-radiation Hydrodynamics Study (2017, methodology): “…processes, we adopt the electron and positron capture of nucleons and heavy nuclei, electron– positron pair annihilation, nucleon–nucleon bremsstrahlung, and plasmon decay based on Fuller et al. (1985), Cooperstein et al. (1986), Burrows et al. (2006), and Ruffert et al. (1996), respectively.”
Colloquium: Perspectives on core-collapse supernova theory (2012, background): “One symptom (or feature) of the problem in 2D may be the long time to explosion seen by, e.g., Marek & Janka 6 translating into a core rotating with ∼1.5- to 4-millisecond periods (2009), Suwa, et al. (2010), Müller, Janka, & Marek (2012), and Burrows et al. (2006).”
Exploring Fundamentally Three-dimensional Phenomena in High-fidelity Simulations of Core-collapse Supernovae (2018, methodology): “For the underlying neutrino interactions, we use isotropic scattering on nucleons, alpha particles, and heavy nuclei following Bruenn (1985); Burrows et al. (2006) with corrections for weak magnetism and recoil from Horowitz (2002).”
AN OPEN-SOURCE NEUTRINO RADIATION HYDRODYNAMICS CODE FOR CORE-COLLAPSE SUPERNOVAE (2014, methodology): “Absorption Cross Sections: NuLib’s neutrino-nucleon charged-current interaction cross sections are taken from Burrows et al. (2006).”
NUCLEAR CONSTRAINTS ON PROPERTIES OF NEUTRON STAR CRUSTS (2009, background): “…observed in X-ray emission following Xray bursts on a neutron star (Duncan 1998), the cooling observed over the first several years following superbursts from neutron stars or giant flares from magnetars (Rutledge et al. 2006), and neutrino opacities (Horowitz et al. 2004; Burrows et al. 2006).”
Global comparison of core-collapse supernova simulations in spherical symmetry (2018, background): “Rather, we determine the emissivity of these processes assuming no final state neutrino blocking (via [73]).”
NEUTRINO SIGNATURES AND THE NEUTRINO-DRIVEN WIND IN BINARY NEUTRON STAR MERGERS (2008, methodology): “The neutrino emission, absorption, and scattering processes used in VULCAN/2D simulations are those summarized in Burrows et al. (2006), and include all the above, plus electron neutrino absorption on nuclei and nucleon-nucleon bremsstrahlung.”
The overarching framework of core-collapse supernova explosions as revealed by 3D fornax simulations (2019, methodology): “Nucleonnucleon bremmstrahlung is handled using the rates found in Thompson et al. (2000) and our approach to e+/e− annihilation into neutrino pairs is found in both Thompson et al. (2000) and Burrows et al. (2006).”
A successful 3D core-collapse supernova explosion model (2018, methodology): “24 of Burrows et al. (2006) and for the charged-current absorption cross sections (i.e., νe + n→ p+ e− and ν̄e + p→ n+ e+) we follow the approach described in sections 3.1 and 3.2 of Burrows et al. (2006).”
The Gravitational Wave Signal from Core-collapse Supernovae (2018, methodology): “We follow the prescription for the neutrino-matter interactions outlined in Burrows et al. (2006).”