Neutron star properties with unified equations of state of dense matter

Fantina, Anthea; Chamel, Nicolas; Pearson, J. M.; Goriely, Stéphane

doi:10.1051/0004-6361/201321884

Cited by 74 publications

(98 citation statements)

References 86 publications

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“…Such models should reproduce not only nuclear masses at best, but also as many experimental observables as possible. These include charge radii and neutron skin thicknesses, fission barriers and shape isomers, spectroscopic data such as the 2 + energies, moments of inertia, but also infinite (neutron and symmetric) nuclear matter properties obtained from realistic calculations as well as specific observed or empirical properties of neutron stars, like their maximum mass or mass-radius relations [23].…”

Section: Nuclear Massesmentioning

confidence: 99%

Towards more accurate and reliable predictions for nuclear applications

Goriely

2015

Eur. Phys. J. A

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Abstract. The need for nuclear data far from the valley of stability, for applications such as nuclear astrophysics or future nuclear facilities, challenges the robustness as well as the predictive power of present nuclear models. Most of the nuclear data evaluation and prediction are still performed on the basis of phenomenological nuclear models. For the last decades, important progress has been achieved in fundamental nuclear physics, making it now feasible to use more reliable, but also more complex microscopic or semimicroscopic models in the evaluation and prediction of nuclear data for practical applications. Nowadays mean-field models can be tuned at the same level of accuracy as the phenomenological models, renormalized on experimental data if needed, and therefore can replace the phenomenological inputs in the evaluation of nuclear data. The latest achievements to determine nuclear masses within the non-relativistic HFB approach, including the related uncertainties in the model predictions, are discussed. Similarly, recent efforts to determine fission observables within the mean-field approach are described and compared with more traditional existing models.

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Section: Nuclear Massesmentioning

confidence: 99%

Towards more accurate and reliable predictions for nuclear applications

Goriely

2015

Eur. Phys. J. A

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“…Consequently, calculating the crust equation of state (EOS) is much less straightforward than for the core, which explains the smaller number of crust EOS available compared to those for the core. In particular, few unified EOS, i.e., those based on the same nuclear model for the crust and core, have been developed; see, for example, Douchin & Haensel (2001), Fantina et al (2013), Pearson et al (2014), Sharma et al (2015), Fortin et al (2016). Therefore non-unified EOS are often used, assuming different nuclear interaction models for the crust and core.…”

Section: Introductionmentioning

confidence: 99%

Neutron star properties and the equation of state for the core

Zdunik

Fortin

Haensel

2017

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Context. Few unified equations of state for neutron star matter, in which core and crust are described using the same nuclear model, are available. However the use of non-unified equations of state with simplified matching between the crust and core has been shown to introduce uncertainties in the radius determination, which can be larger than the expected precision of the next generation of X-ray satellites. Aims. We aim to eliminate the dependence of the radius and mass of neutron stars on the detailed model for the crust and on the crust-core matching procedure. Methods. We solved the approximate equations of the hydrostatic equilibrium for the crust of neutron stars and obtained a precise formula for the radius that only depends on the core mass and radius, the baryon chemical potential at the core-crust interface, and at the crust surface. For a fully accreted crust one needs, additionally, the value of the total deep crustal heating per one accreted nucleon. Results. For typical neutron star masses, the approximate approach allows us to determine the neutron star radius with an error ∼0.1% (∼10 m, equivalent to a 1% inaccuracy in the crust thickness). The formalism applies to neutron stars with a catalyzed or a fully accreted crust. The difference in the neutron star radius between the two models is proportional to the total energy release due to deep crustal heating. Conclusions. For a given model of dense matter describing the neutron star core, the radius of a neutron star can be accurately determined independent of the crust model with a precision much better than the ∼5% precision expected from the next generation of X-ray satellites. This allows us to circumvent the problem of the radius uncertainty that may arise when non-unified equations of state for the crust and core are used.

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“…However, it is worth pointing out that, within the constraint provided by the observation of a 2 solar masses neutron star, the shift symmetric Horndeski model that we consider is still compatible with surface redshift observations, so there is no tension. More specifically, we find that neutron stars with masses in the conservative range of 1.3 − 1.5M are compatible with surface redshift in the range z = 0.23 ± 0.07, using equations of state that are not excluded in GR, [54].…”

Section: A Gamma Ray Burst Repeater Redshiftmentioning

confidence: 79%

“…Some additional tests are discussed in [54]. The reliability of the EOSs is summarized in Even if some of the EOSs we use are disfavored within GR, we will include them in our study for completeness.…”

Section: Slowly Rotating Neutron Starsmentioning

confidence: 99%

“…This constraint emerges again by expanding the equations of motion 7 It is expected that this result no longer holds at higher order in the expansion. [54], the BSK14 and eosL statuses are based on the ability to reproduce a 2 M neutron star within GR. The column 'reliability' is a qualitative level of reliability used in this paper: +, ±, and − indicate respectively reliable, marginally reliable and not reliable.…”

Section: Slowly Rotating Neutron Starsmentioning

confidence: 99%

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Slowly rotating neutron stars in the nonminimal derivative coupling sector of Horndeski gravity

et al. 2016

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This work is devoted to the construction of slowly rotating neutron stars in the framework of the nonminimal derivative coupling sector of Horndeski theory. We match the large radius expansion of spherically symmetric solutions with cosmological solutions and we find that the most viable model has only one free parameter. Then, by using several tabulated and realistic equations of state, we establish numerically the upper bound for this parameter in order to construct neutron stars in the slow rotation approximation with the maximal mass observed today. We finally study the surface redshift and the inertia of these objects and compare them with known data.

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Neutron star properties with unified equations of state of dense matter

Cited by 74 publications

References 86 publications

Towards more accurate and reliable predictions for nuclear applications

Towards more accurate and reliable predictions for nuclear applications

Neutron star properties and the equation of state for the core

Slowly rotating neutron stars in the nonminimal derivative coupling sector of Horndeski gravity

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