Existence of hyperons in the pulsar PSRJ1614-2230

Sulaksono, A.; Agrawal, B. K.

doi:10.1016/j.nuclphysa.2012.09.006

Cited by 53 publications

(64 citation statements)

References 43 publications

(67 reference statements)

Supporting

Mentioning

Contrasting

Unclassified

Order By: Relevance

“…We also note that the neutron star EOS found in the literature is mostly thermodynamically consistent and it is also well known that the neutron star matter with stiffer EOS predicts a higher maximum mass (see, e.g., Ref. [20] and references therein).…”

supporting

confidence: 71%

Bosons star at finite temperature

2014

Self Cite

View full text Add to dashboard Cite

By using a simple thermodynamical method we confirm the finding of Chavanis and Harko that stable Bose-Einstein condensate stars can form. However, by using a thermodynamically consistent boson equation of state, we obtain a less massive Bose-Einstein condensate star compared to the one predicted by Chavanis and Harko. We also obtain that the maximum mass of a boson star is insensitive to the change of matter temperature. However, the mass of boson star with relatively large radius depends significantly on the temperature of the boson matter.

show abstract

supporting

confidence: 71%

Bosons star at finite temperature

2014

Self Cite

View full text Add to dashboard Cite

show abstract

“…53 Simultaneously, some relativistic mean-field (RMF) calculations including hyperons can support NSs as massive as PSR J1614−2230. [54][55][56][57][58][59][60] This discrepancy can be understood at least partly from the fact that the maximum mass depends very sensitively on the various hyperonic couplings, and these are determined very poorly since the limited nuclear and hypernuclear data constrain the EoS only in the vicinity of the saturation density, whereas the maximum NS mass is mostly determined by the EoS at much higher densities (typically between ∼ 5ρ 0 and 10ρ 0 ). Indeed, it has been shown that to obtain M max > 2 M one has to introduce an additional high-density repulsion between hyperons, due to the exchange of the hidden-strangeness φ meson.…”

Section: Hyperonic Inner Corementioning

confidence: 99%

On the Maximum Mass of Neutron Stars

Chamel

Haensel

Zdunik

et al. 2013

Int. J. Mod. Phys. E

View full text Add to dashboard Cite

show abstract

“…The nucleonic models, the so-called noY models, include the scalar σ , vector ω, and vector-isovector ρ meson fields (possibly also the δ meson) together with the nucleon doublet: neutron n and proton p. The Y and Yss models denote hyperonic EOS and, with respect to the noY models, they also include the six lightest hyperons ( 0 , the + , 0 , − triplet, and the 0 , − doublet) and the hidden-strangeness vector-isoscalar φ meson for the Y models, or the φ meson together with the hidden-strangeness scalar-isoscalar σ * for the Yss models. The vector meson-hyperon coupling constants are always calculated assuming SU(6) symmetry (see, e.g., [56][57][58]):…”

Section: A Rmf Unified Eosmentioning

confidence: 99%

Neutron star radii and crusts: Uncertainties and unified equations of state

Fortin¹,

Providência²,

Raduta³

et al. 2016

Phys. Rev. C

313

377

View full text Add to dashboard Cite

The uncertainties in neutron star radii and crust properties due to our limited knowledge of the equation of state are quantitatively analyzed. We first demonstrate the importance of a unified microscopic description for the different baryonic densities of the star. If the pressure functional is obtained matching a crust and a core equation of state based on models with different properties at nuclear matter saturation, the uncertainties can be as large as ∼30 % for the crust thickness and 4% for the radius. Necessary conditions for causal and thermodynamically consistent matchings between the core and the crust are formulated and their consequences examined. A large set of unified equations of state for purely nucleonic matter is obtained based on twenty-four Skyrme interactions and nine relativistic mean-field nuclear parametrizations. In addition, for relativistic models fifteen equations of state including a transition to hyperonic matter at high density are presented. All these equations of state have in common the property of describing a 2M star and of being causal within stable neutron stars. Spans of ∼3 and ∼4 km are obtained for the radius of, respectively, 1.0M and 2.0M stars. Applying a set of nine further constraints from experiment and ab initio calculations the uncertainty is reduced to ∼1 and 2 km, respectively. These residual uncertainties reflect lack of constraints at large densities and insufficient information on the density dependence of the equation of state near the nuclear matter saturation point. The most important parameter to be constrained is shown to be the symmetry energy slope L. Indeed, this parameter exhibits a linear correlation with the stellar radius, which is particularly clear for small mass stars around 1.0M . The other equation-of-state parameters do not show clear correlations with the radius, within the present uncertainties. Potential constraints on L, the neutron star radius, and the equation of state from observations of thermal states of neutron stars are also discussed. The unified equations of state are made available in the Supplemental Materials and via the CompOSE database.

show abstract

Existence of hyperons in the pulsar PSRJ1614-2230

Cited by 53 publications

References 43 publications

Bosons star at finite temperature

Bosons star at finite temperature

On the Maximum Mass of Neutron Stars

Neutron star radii and crusts: Uncertainties and unified equations of state

Contact Info

Product

Resources

About