A two-solar-mass neutron star measured using Shapiro delay

Demorest, Paul; Pennucci, T. T.; Ransom, S. M.; Roberts, M. S. E.; Hessels, J. W. T.

doi:10.1038/nature09466

Cited by 3,948 publications

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“…1, the horizontal bands represent the masses of the heavy NSs PSR J1614-2230 [1] and PSR J0348+0432 [2]. The maximum masses of hyperonic NSs with the present EOSs are well below those observational data, even in the case of the most repulsive odd-state ΛΛ interaction (Type 4).…”

Section: Numerical Results and Discussionmentioning

confidence: 72%

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Variational Approach to Neutron Star Matter with Hyperons

Togashi¹,

Hiyama²,

Yamamoto³

et al. 2017

Proceedings of the 12th International Conference on Hypernuclear and Strange Particle Physics (HYP2015)

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Equations of state (EOSs) for uniform nuclear matter including Λ and Σ − hyperons are constructed with the variational method starting from the bare baryon interactions to study the structure and composition of neutron stars (NSs). For the nucleon sector, the Argonne v18 two-nucleon potential and the Urbana IX three-nucleon potential are adopted. On the other hand, for the hyperon sector, central two-body potentials that reproduce the experimental data on hypernuclei are employed as the Λ-nucleon, Σ − -nucleon and ΛΛ interactions. Since there are no experimental data on the odd-state component of the ΛΛ interaction, we prepare four odd-state ΛΛ interaction models, and calculate four EOSs of hyperonic nuclear matter for those interactions using the cluster variational method. The obtained maximum mass of NSs increases as the odd-state ΛΛ interaction becomes more repulsive, although it is still smaller than the recently observed masses of heavy NSs. Moreover, the critical density of Σ − strongly depends on the odd-state ΛΛ interaction. A phenomenological three-baryon repulsive force is employed in our variational calculations to explain the observed data on heavy NSs.

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Section: Numerical Results and Discussionmentioning

confidence: 72%

“…Recent observational data on the masses of PSR J1614-2230 (M = 1.97 ± 0.04M ⊙ ) [1] and PSR J0348+0432 (M = 2.01 ± 0.04M ⊙ ) [2] provide severe constraints on the nuclear EOS. In particular, these heavy NSs are difficult to explain when hyperon mixing in NSs is considered.…”

Section: Introductionmentioning

confidence: 99%

Variational Approach to Neutron Star Matter with Hyperons

Togashi¹,

Hiyama²,

Yamamoto³

et al. 2017

Proceedings of the 12th International Conference on Hypernuclear and Strange Particle Physics (HYP2015)

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“…The resulting hadronic NS have maximum masses of less than about 1.4 M , and the presence of quark matter inside the star is required in order to reach larger values. It remains to be seen which values of the maximum mass can be reached with more sophisticated quark matter models in the future, in particular with respect to the recent claim of discovery of a two solar mass NS [27].…”

Section: Discussionmentioning

confidence: 99%

Neutron Star Structure with Hyperons and Quarks

Schulze¹

2015

Proceedings of the International Symposium “Nanoscience and Quantum Physics 2012” (nanoPHYS’12)

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The high-density nuclear equation of state within the Brueckner-Hartree-Fock approach is discussed, with particular attention to the effects of nucleonic three-body forces, the presence of hyperons, and the joining with an eventual quark matter phase. The resulting properties of neutron stars, in particular the mass-radius relation, are determined. It turns out that in this approach stars heavier than about 1.4 solar masses contain necessarily quark matter.

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“…We assume that the entire quark matter is in the CSC phase with large energy gap ∆ ≥ 10 MeV. The maximum mass with this EoS is 2.13M ⊙ , and it satisfies recent 2M ⊙ observations [5,6]. We select the stellar masses of neutron stars to be 1.41, 2.04, and 2.13M ⊙ .…”

Section: Cooling Modelmentioning

confidence: 99%

Neutron Star Cooling with Various Superfluid and Superconducting States

Noda¹,

Hashimoto²,

Matsuo³

et al. 2017

Proceedings of the 14th International Symposium on Nuclei in the Cosmos (NIC2016)

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A neutron star is a highly dense object which lasts after a supernova explosion. The density of a neutron star overcomes the nuclear density, and the temperature is high at the beginning of its history. An isolated neutron star does not have any heat sources, and it cools down emitting thermal energy by neutrinos. The neutrino emission process depends on the state of interior matter of the neutron star. To compare theoretical simulations and observations of neutron stars, it can constrain the nuclear theory of high density region. We create a model of neutron stars with colour superconducting quark matter and nucleon superfluidity / superconductivity, to satisfy recent observations, including two 2M ⊙ neutron stars. We parameterize these super-states and demonstrate the cooling curves, which show heavy stars do not always cool faster than lighter stars.

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A two-solar-mass neutron star measured using Shapiro delay

Cited by 3,948 publications

References 24 publications

Variational Approach to Neutron Star Matter with Hyperons

Variational Approach to Neutron Star Matter with Hyperons

Neutron Star Structure with Hyperons and Quarks

Neutron Star Cooling with Various Superfluid and Superconducting States

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