Cooling Timescale for Protoneutron Stars and Properties of Nuclear Matter

Effective Mass and Symmetry Energy at High Densities

Kenichiro Nakazato, Hideyuki Suzuki

Research output: Contribution to journalArticle

2 Citations (Scopus)

Abstract

The cooling process of a protoneutron star (PNS) is investigated with focus on its sensitivity to properties of hot and dense matter. An equation of state, which includes the nucleon effective mass and nuclear symmetry energy at twice the saturation density as control parameters, is constructed for systematic studies. The numerical code utilized in this study follows a quasi-static evolution of a PNS solving the general-relativistic stellar structure with neutrino diffusion. The cooling timescale evaluated from the neutrino light curve is found to be longer for the models with larger effective masses and smaller symmetry energies at high densities. The present results are compared with those for other equations of state and it is found that they are consistent in terms of their dependences on the effective mass and neutron star radius.

Original languageEnglish
Article number25
JournalAstrophysical Journal
Volume878
Issue number1
DOIs
Publication statusPublished - Jun 10 2019

Fingerprint

symmetry
cooling
timescale
equation of state
stars
equations of state
neutrinos
stellar structure
energy
neutron stars
light curve
saturation
radii
sensitivity
code
parameter

All Science Journal Classification (ASJC) codes

  • Astronomy and Astrophysics
  • Space and Planetary Science

Cite this

Cooling Timescale for Protoneutron Stars and Properties of Nuclear Matter : Effective Mass and Symmetry Energy at High Densities. / Nakazato, Kenichiro; Suzuki, Hideyuki.

In: Astrophysical Journal, Vol. 878, No. 1, 25, 10.06.2019.

Research output: Contribution to journalArticle

@article{c6fa8efe01e74cd0b3c42f2a1fd4bc15,
title = "Cooling Timescale for Protoneutron Stars and Properties of Nuclear Matter: Effective Mass and Symmetry Energy at High Densities",
abstract = "The cooling process of a protoneutron star (PNS) is investigated with focus on its sensitivity to properties of hot and dense matter. An equation of state, which includes the nucleon effective mass and nuclear symmetry energy at twice the saturation density as control parameters, is constructed for systematic studies. The numerical code utilized in this study follows a quasi-static evolution of a PNS solving the general-relativistic stellar structure with neutrino diffusion. The cooling timescale evaluated from the neutrino light curve is found to be longer for the models with larger effective masses and smaller symmetry energies at high densities. The present results are compared with those for other equations of state and it is found that they are consistent in terms of their dependences on the effective mass and neutron star radius.",
author = "Kenichiro Nakazato and Hideyuki Suzuki",
year = "2019",
month = "6",
day = "10",
doi = "10.3847/1538-4357/ab1d4b",
language = "English",
volume = "878",
journal = "Astrophysical Journal",
issn = "0004-637X",
publisher = "IOP Publishing Ltd.",
number = "1",

}

TY - JOUR

T1 - Cooling Timescale for Protoneutron Stars and Properties of Nuclear Matter

T2 - Effective Mass and Symmetry Energy at High Densities

AU - Nakazato, Kenichiro

AU - Suzuki, Hideyuki

PY - 2019/6/10

Y1 - 2019/6/10

N2 - The cooling process of a protoneutron star (PNS) is investigated with focus on its sensitivity to properties of hot and dense matter. An equation of state, which includes the nucleon effective mass and nuclear symmetry energy at twice the saturation density as control parameters, is constructed for systematic studies. The numerical code utilized in this study follows a quasi-static evolution of a PNS solving the general-relativistic stellar structure with neutrino diffusion. The cooling timescale evaluated from the neutrino light curve is found to be longer for the models with larger effective masses and smaller symmetry energies at high densities. The present results are compared with those for other equations of state and it is found that they are consistent in terms of their dependences on the effective mass and neutron star radius.

AB - The cooling process of a protoneutron star (PNS) is investigated with focus on its sensitivity to properties of hot and dense matter. An equation of state, which includes the nucleon effective mass and nuclear symmetry energy at twice the saturation density as control parameters, is constructed for systematic studies. The numerical code utilized in this study follows a quasi-static evolution of a PNS solving the general-relativistic stellar structure with neutrino diffusion. The cooling timescale evaluated from the neutrino light curve is found to be longer for the models with larger effective masses and smaller symmetry energies at high densities. The present results are compared with those for other equations of state and it is found that they are consistent in terms of their dependences on the effective mass and neutron star radius.

UR - http://www.scopus.com/inward/record.url?scp=85069483911&partnerID=8YFLogxK

UR - http://www.scopus.com/inward/citedby.url?scp=85069483911&partnerID=8YFLogxK

U2 - 10.3847/1538-4357/ab1d4b

DO - 10.3847/1538-4357/ab1d4b

M3 - Article

VL - 878

JO - Astrophysical Journal

JF - Astrophysical Journal

SN - 0004-637X

IS - 1

M1 - 25

ER -