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Spin-polarized β-stable neutron star matter: the nuclear symmetry energy and GW170817 constraint

Magnetic field of rotating pulsar might be so strong that the equation of state (EOS) of neutron star (NS) matter is significantly affected by the spin polarization of baryons. In the present work, the EOS of the spin-polarized nuclear matter is investigated in the nonrelativistic Hartree-Fock forma...

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Main Authors: Ngo Hai Tan, ,, Dao T. Khoa, Doan Thi Loan
Format: Article
Language:English
Published: 2020
Subjects:
High Energy Astrophysical Phenomena (astro-ph.HE)
Nuclear Experiment (nucl-ex)
Nuclear Theory (nucl-th)
Online Access:https://dlib.phenikaa-uni.edu.vn/handle/PNK/585
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spelling oai:localhost:PNK-5852022-08-17T05:54:37Z Spin-polarized β-stable neutron star matter: the nuclear symmetry energy and GW170817 constraint Ngo Hai Tan, , Dao T. Khoa Doan Thi Loan High Energy Astrophysical Phenomena (astro-ph.HE) Nuclear Experiment (nucl-ex) Nuclear Theory (nucl-th) Magnetic field of rotating pulsar might be so strong that the equation of state (EOS) of neutron star (NS) matter is significantly affected by the spin polarization of baryons. In the present work, the EOS of the spin-polarized nuclear matter is investigated in the nonrelativistic Hartree-Fock formalism, using a realistic density dependent nucleon-nucleon interaction with its spin and spin-isospin dependence accurately adjusted to the Brueckner-Hartree-Fock results for the spin-polarized nuclear matter. The nuclear symmetry energy and proton fraction are found to increase significantly with the increasing spin polarization of baryons, leading to a larger probability of the direct Urca process in the cooling of magnetar. The EOS of the β-stable npeμ matter obtained at different spin polarizations of baryons is used as the input for the Tolman-Oppenheimer-Volkov equations to determine the hydrostatic configuration of NS. Based on the GW170817 constraint on the radius R1.4 of NS with M≈1.4⊙, our mean-field results show that up to 60 % of baryons in the NS merger might be spin-polarized. This result supports the magnetar origin of the blue kilonova ejecta of GW170817 suggested by Metzger et al., and the spin polarization of baryons needs, therefore, to be properly treated in the many-body calculation of the EOS of NS matter before comparing the calculated NS mass and radius with those constrained by the multi-messenger GW170817 observation. 2020-10-13T04:13:43Z 2020-10-13T04:13:43Z 2020 Article Working Paper arXiv:2010.00869 arXiv:2010.00869v1 https://dlib.phenikaa-uni.edu.vn/handle/PNK/585 en application/pdf
institution Digital Phenikaa
collection Digital Phenikaa
language English
topic High Energy Astrophysical Phenomena (astro-ph.HE)
Nuclear Experiment (nucl-ex)
Nuclear Theory (nucl-th)
spellingShingle High Energy Astrophysical Phenomena (astro-ph.HE)
Nuclear Experiment (nucl-ex)
Nuclear Theory (nucl-th)
Ngo Hai Tan, ,
Dao T. Khoa
Doan Thi Loan
Spin-polarized β-stable neutron star matter: the nuclear symmetry energy and GW170817 constraint
description Magnetic field of rotating pulsar might be so strong that the equation of state (EOS) of neutron star (NS) matter is significantly affected by the spin polarization of baryons. In the present work, the EOS of the spin-polarized nuclear matter is investigated in the nonrelativistic Hartree-Fock formalism, using a realistic density dependent nucleon-nucleon interaction with its spin and spin-isospin dependence accurately adjusted to the Brueckner-Hartree-Fock results for the spin-polarized nuclear matter. The nuclear symmetry energy and proton fraction are found to increase significantly with the increasing spin polarization of baryons, leading to a larger probability of the direct Urca process in the cooling of magnetar. The EOS of the β-stable npeμ matter obtained at different spin polarizations of baryons is used as the input for the Tolman-Oppenheimer-Volkov equations to determine the hydrostatic configuration of NS. Based on the GW170817 constraint on the radius R1.4 of NS with M≈1.4⊙, our mean-field results show that up to 60 % of baryons in the NS merger might be spin-polarized. This result supports the magnetar origin of the blue kilonova ejecta of GW170817 suggested by Metzger et al., and the spin polarization of baryons needs, therefore, to be properly treated in the many-body calculation of the EOS of NS matter before comparing the calculated NS mass and radius with those constrained by the multi-messenger GW170817 observation.
format Article
author Ngo Hai Tan, ,
Dao T. Khoa
Doan Thi Loan
author_facet Ngo Hai Tan, ,
Dao T. Khoa
Doan Thi Loan
author_sort Ngo Hai Tan, ,
title Spin-polarized β-stable neutron star matter: the nuclear symmetry energy and GW170817 constraint
title_short Spin-polarized β-stable neutron star matter: the nuclear symmetry energy and GW170817 constraint
title_full Spin-polarized β-stable neutron star matter: the nuclear symmetry energy and GW170817 constraint
title_fullStr Spin-polarized β-stable neutron star matter: the nuclear symmetry energy and GW170817 constraint
title_full_unstemmed Spin-polarized β-stable neutron star matter: the nuclear symmetry energy and GW170817 constraint
title_sort spin-polarized β-stable neutron star matter: the nuclear symmetry energy and gw170817 constraint
publishDate 2020
url https://dlib.phenikaa-uni.edu.vn/handle/PNK/585
_version_ 1751856315846623232
score 8.887836

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