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Proto-neutron star evolution with improved charged-current neutrino-nucleon interactions

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arxiv 2201.01955 v1 pith:HL6POPLV submitted 2022-01-06 nucl-th astro-ph.HE

A Pascal (LUTH (UMR_8102)) , J Novak (LUTH (UMR_8102)) , M Oertel (LUTH (UMR_8102)) This is my paper
classification nucl-thastro-ph.HE
keywords approximationneutrino-nucleoncharged-currentconvectivecoolingcorrelationsinclusionnuclear
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We perform simulations of the Kelvin-Helmholtz cooling phase of proto-neutron stars with a new numerical code in spherical symmetry and using the quasi-static approximation. We use for the first time the full set of charged-current neutrino-nucleon reactions, including neutron decay and modified Urca processes, together with the energy-dependent numerical representation for the inclusion of nuclear correlations with random-phase approximation. Moreover, convective motions are taken into account within the mixing-length theory. As we vary the assumptions for computing neutrino-nucleon reaction rates, we show that the dominant effect on the cooling timescale, neutrino signal and composition of the neutrino-driven wind comes from the inclusion of convective motion. Computation of nuclear correlations within the random phase approximation, as compared to mean field approach, has a relatively small impact.

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Cited by 3 Pith papers

Reviewed papers in the Pith corpus that reference this work. Sorted by Pith novelty score. Full citation record

  1. Solar-System Abundances of $p$-Nuclides Probe Collective Neutrino Oscillations in Supernovae

    hep-ph 2026-07 conditional novelty 6.0 of 10

    Nearby neutrino flavor conversion in a supernova can boost νp-process yields of p-nuclides like 92Mo and 92Nb by up to two orders of magnitude, matching solar abundances when conversion starts within ~10 km of the pro...

  2. The petit four of color-superconducting phases in proto-neutron star evolution

    nucl-th 2026-07 conditional novelty 6.0 of 10

    Along constant-baryon-number cooling tracks, color-superconducting cores in proto-neutron stars follow four scenarios, with stable cold CSC only in a narrow high-mass band for the chosen EoS.

  3. Electron-neutrino lepton number crossings: Variations with the supernova core physics

    astro-ph.HE 2025-07 conditional novelty 6.0 of 10

    In a suite of 12 supernova models, electron-neutrino lepton number crossings appear at larger radii when proto-neutron star convection is included and at smaller radii when muon production is included.

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