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Title: Evolution of a proto-neutron star with a nuclear many-body equation of state: Neutrino luminosity and gravitational wave frequencies

Abstract

In a core-collapse supernova, a huge amount of energy is released in the Kelvin-Helmholtz phase subsequent to the explosion, when the proto-neutron star cools and deleptonizes as it loses neutrinos. Most of this energy is emitted through neutrinos, but a fraction of it can be released through gravitational waves. We model the evolution of a proto-neutron star in the Kelvin-Helmholtz phase using a general relativistic numerical code, and a recently proposed finite temperature, many-body equation of state; from this we consistently compute the diffusion coefficients driving the evolution. To include the many-body equation of state, we develop a new fitting formula for the high density baryon free energy at finite temperature and intermediate proton fraction. Here, we estimate the emitted neutrino signal, assessing its detectability by present terrestrial detectors, and we determine the frequencies and damping times of the quasinormal modes which would characterize the gravitational wave signal emitted in this stage.

Authors:
 [1];  [2];  [3];  [3];  [4];  [3]
  1. Univ. di Roma, Roma (Italy). Dipartimento di Fisica; Stockholm Univ. (Sweden). Astronomy and Oskar Klein Centre
  2. Argonne National Lab. (ANL), Argonne, IL (United States). Physics Division
  3. Univ. di Roma, Roma (Italy). Dipartimento di Fisica
  4. Univ. d'Alacant, Alacant (Spain). Dept. de Fisica Aplicada
Publication Date:
Research Org.:
Argonne National Lab. (ANL), Argonne, IL (United States)
Sponsoring Org.:
USDOE Office of Science (SC), Nuclear Physics (NP)
OSTI Identifier:
1415938
Alternate Identifier(s):
OSTI ID: 1377655
Grant/Contract Number:  
AC02-06CH11357; StronGrHEP-690904; AYA2015-66899-C2-2-P
Resource Type:
Accepted Manuscript
Journal Name:
Physical Review D
Additional Journal Information:
Journal Volume: 96; Journal Issue: 4; Journal ID: ISSN 2470-0010
Publisher:
American Physical Society (APS)
Country of Publication:
United States
Language:
English
Subject:
79 ASTRONOMY AND ASTROPHYSICS; Supernovae; Stars; Gravitational waves

Citation Formats

Camelio, Giovanni, Lovato, Alessandro, Gualtieri, Leonardo, Benhar, Omar, Pons, José A., and Ferrari, Valeria. Evolution of a proto-neutron star with a nuclear many-body equation of state: Neutrino luminosity and gravitational wave frequencies. United States: N. p., 2017. Web. https://doi.org/10.1103/PhysRevD.96.043015.
Camelio, Giovanni, Lovato, Alessandro, Gualtieri, Leonardo, Benhar, Omar, Pons, José A., & Ferrari, Valeria. Evolution of a proto-neutron star with a nuclear many-body equation of state: Neutrino luminosity and gravitational wave frequencies. United States. https://doi.org/10.1103/PhysRevD.96.043015
Camelio, Giovanni, Lovato, Alessandro, Gualtieri, Leonardo, Benhar, Omar, Pons, José A., and Ferrari, Valeria. Wed . "Evolution of a proto-neutron star with a nuclear many-body equation of state: Neutrino luminosity and gravitational wave frequencies". United States. https://doi.org/10.1103/PhysRevD.96.043015. https://www.osti.gov/servlets/purl/1415938.
@article{osti_1415938,
title = {Evolution of a proto-neutron star with a nuclear many-body equation of state: Neutrino luminosity and gravitational wave frequencies},
author = {Camelio, Giovanni and Lovato, Alessandro and Gualtieri, Leonardo and Benhar, Omar and Pons, José A. and Ferrari, Valeria},
abstractNote = {In a core-collapse supernova, a huge amount of energy is released in the Kelvin-Helmholtz phase subsequent to the explosion, when the proto-neutron star cools and deleptonizes as it loses neutrinos. Most of this energy is emitted through neutrinos, but a fraction of it can be released through gravitational waves. We model the evolution of a proto-neutron star in the Kelvin-Helmholtz phase using a general relativistic numerical code, and a recently proposed finite temperature, many-body equation of state; from this we consistently compute the diffusion coefficients driving the evolution. To include the many-body equation of state, we develop a new fitting formula for the high density baryon free energy at finite temperature and intermediate proton fraction. Here, we estimate the emitted neutrino signal, assessing its detectability by present terrestrial detectors, and we determine the frequencies and damping times of the quasinormal modes which would characterize the gravitational wave signal emitted in this stage.},
doi = {10.1103/PhysRevD.96.043015},
journal = {Physical Review D},
number = 4,
volume = 96,
place = {United States},
year = {2017},
month = {8}
}

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Cited by: 10 works
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