The pasta phase and its consequences on neutrino opacities

Abstract

In this paper, we calculate the diffusion coefficients that are related to the neutrino opacities considering the formation of nuclear pasta and homogeneous matter at low densities. Our results show that the mean free paths are significantly altered by the presence of nuclear pasta in stellar matter when compared with the results obtained with homogeneous matter. These differences in neutrino opacities certainly influence the Kelvin-Helmholtz phase of protoneutron stars and consequently the results of supernova explosion simulations.

References in corpus (21)

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Cited by in corpus (22)

• Disordered nuclear pasta, magnetic field decay, and crust cooling in neutron stars
• The influence of strong magnetic fields on proto-quark stars
• A Minimal Nuclear Energy Density Functional
• Nuclear Waffles
• Quantum Nuclear Pasta and Nuclear Symmetry Energy
• Stability windows for proto-quark stars
• Neutrinos and nucleosynthesis of elements
• A Neutron Star is born
• Domains and defects in nuclear "pasta"
• Neutron stars: from the inner crust to the core with the (Extended) Nambu-Jona-Lasinio model
• Is the magnetic field making the inner crust of neutron stars more heterogeneous?
• Nuclear pasta structures and symmetry energy
• Pasta phases within the QMC model
• Nuclear pasta and supernova neutrinos at late times
• Pasta fluctuations in symmetric matter at finite temperature
• Anisotropic electron transport in the nuclear pasta phase
• Neutrino diffusion in the pasta phase matter within the Thomas-Fermi approach
• Nuclear pasta structures at high temperatures
• Strange quark matter and proto-strange stars in an equivaparticle model
• Elasticity of neutron star mantle: improved compressible liquid drop model for cylindrical phases
• Do short range correlations inhibit the appearance of the nuclear pasta?
• Tasting Nuclear Pasta Made with Classical Molecular Dynamics Simulations