Hyperonic neutron star matter in light of GW170817

Since 2013, the mass of pulsar PSR J0348 + 0432 (M = 2.01M⊙) has provided a tight constraint on neutron star (NS) equation of state. However, a number of different analyses of the recently detected binary neutron star (BNS) merger (GW170817) point to a maximum NS mass around 2.16M⊙. In addition, a r...

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Bibliographic Details
Published in:Astronomische Nachrichten 2019-01, Vol.340 (1-3), p.145-150
Main Authors: Spinella, W. M., Weber, F.
Format: Article
Language:English
Subjects:
Binary stars
Constants
Coupling
Empirical analysis
equation of state
Equations of state
gravitational waves
Hypernuclei
Hyperons
Mathematical analysis
Millisecond pulsars
Neutron stars
Neutrons
stars: neutron
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Summary:Since 2013, the mass of pulsar PSR J0348 + 0432 (M = 2.01M⊙) has provided a tight constraint on neutron star (NS) equation of state. However, a number of different analyses of the recently detected binary neutron star (BNS) merger (GW170817) point to a maximum NS mass around 2.16M⊙. In addition, a recent study determined the mass of the millisecond pulsar PSR J2215 + 5135 to be 2.27−0.15+0.17M⊙. In this work, we investigate the presence of hyperons in NS matter in light of these new mass measurements using equations of state calculated in the relativistic mean‐field approximation. Particular attention is paid to the use of the available empirical data from the study of hypernuclei and that of the SU(3) symmetry relations in fixing the meson‐hyperon coupling constants. We find that hyperonic equations of state with reasonable choices for the meson‐hyperon coupling constants can satisfy these new mass constraints, with hyperons potentially accounting for more than 10% of the baryons in the core of a NS.
ISSN:0004-6337
1521-3994
DOI:10.1002/asna.201913579