Nuclear energy density functional and the nuclear 
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 decay

Lim, Yeunhwan; Oh, Yongseok

doi:10.1103/physrevc.95.034311

Cited by 12 publications

(20 citation statements)

References 57 publications

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“…16 summarizes several of the constraints on the neutron skin thickness of 208 Pb from both nuclear experiment and mean field model calculations. For the mean field theory calculations, we obtained [72,125] Skyrme parameters fitted to the neutron matter equation of state from chiral effective field theory [76,78] and the binding energies of doubly-closed-shell nuclei. From nuclear experiments, we see that the overlapping region of neutron skin has the boundary, 0.16 < ∆ R np < 0.18 fm, which implies that 40 ≤ L ≤ 60 MeV.…”

Section: Resultsmentioning

confidence: 99%

“…A common framework is to employ polytropic equations of state [64][65][66][67], which have the freedom to change the adiabatic index and account for the possibility of phase transitions at specified densities. In addition, Skyrme Hartee-Fock or relativistic mean field (RMF) models [40,[68][69][70][71][72], whose parameters are fitted to the properties of finite nuclei close to saturation density, are generally extrapolated to much higher densities in order to study the mass-radius relationship for neutron stars.…”

Section: Equation Of Statementioning

confidence: 99%

“…The inhomogeneous nuclear matter in the crust of a neutron star represents a phase co-existence problem between dense and dilute matter [72]. The density of the heavy nucleus corresponds to the dense phase while the unbound neutrons correspond to the dilute phase.…”

Section: Neutron Star Crustmentioning

confidence: 99%

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Bayesian modeling of the nuclear equation of state for neutron star tidal deformabilities and GW170817

Lim¹,

Holt²

2019

Eur. Phys. J. A

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We present predictions for neutron star tidal deformabilities obtained from a Bayesian analysis of the nuclear equation of state, assuming a minimal model at high-density that neglects the possibility of phase transitions. The Bayesian posterior probability distribution is constructed from priors obtained from microscopic many-body theory based on realistic two-and three-body nuclear forces, while the likelihood functions incorporate empirical information about the equation of state from nuclear experiments. The neutron star crust equation of state is constructed from the liquid drop model, and the core-crust transition density is found by comparing the energy per baryon in inhomogeneous matter and uniform nuclear matter. From the cold β -equilibrated neutron star equation of state, we then compute neutron star tidal deformabilities as well as the mass-radius relationship. Finally, we investigate correlations between the neutron star tidal deformability and properties of finite nuclei.

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Section: Resultsmentioning

confidence: 99%

Section: Equation Of Statementioning

confidence: 99%

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Bayesian modeling of the nuclear equation of state for neutron star tidal deformabilities and GW170817

Lim¹,

Holt²

2019

Eur. Phys. J. A

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“…Note that we use the same energy density functional for f i and f no as used in the bulk matter EOS. By applying the Lagrange multiplier method with the constraints for baryon and charge number density, we have [82]…”

Section: Parameterized Nuclear Energy Density Functionalmentioning

confidence: 99%

Predicting the moment of inertia of pulsar J0737-3039A from Bayesian modeling of the nuclear equation of state

2019

Self Cite

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We investigate neutron star moments of inertia from Bayesian posterior probability distributions of the nuclear equation of state that incorporate information from microscopic many-body theory and empirical data of finite nuclei. We focus on PSR J0737-3039A and predict that for this 1.338 M neutron star the moment of inertia lies in the range 1.04 × 10 45 g cm 2 < I < 1.51 × 10 45 g cm 2 at the 95% credibility level, while the most probable value for the moment of inertia isĨ = 1.36×10 45 g cm 2 . Assuming a measurement of the PSR J0737-3039A moment of inertia to 10% precision, we study the implications for neutron star radii and tidal deformabilities. We also determine the crustal component of the moment of inertia and find that for typical neutron star masses 1.3M < M < 1.5M the crust contributes 1 − 6% of the total moment of inertia, below what is needed to explain large pulsar glitches in the scenario of strong neutron entrainment.

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“…In the second case there is a significant free neutron fraction Y n ≈ 0.8 and a broad neutron distribution is clearly seen. We refer the reader to References [35,44] and more recent works [62,[65][66][67] for a detailed discussion of the inner crust composition in the absence of accretion.…”

Section: Pristine Crust Compositionmentioning

confidence: 99%

Nuclear physics of the outer layers of accreting neutron stars

Meisel

Deibel

Keek

et al. 2018

J. Phys. G: Nucl. Part. Phys.

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Now 50 years since the existence of the neutron star crust was proposed, we review the current understanding of the nuclear physics of the outer layers of accreting neutron stars. Nuclei produced during nuclear burning replace the nascent composition of the neutron star ocean and crust. Non-equilibrium nuclear reactions driven by compression alter the outer thermal structure and chemical composition, leaving observable imprints on astronomical phenomena. As observations of bursting neutron stars and cooling neutron stars have increased, the recent volume of astronomical data allows new insights into the microphysics of the neutron star interior and the possibility to test nuclear physics input in model calculations. Despite numerous advances in our understanding of neutron star interiors and observed neutron star phenomena, many challenges remain in the astrophysics theory of accreting neutron stars, the nuclear theory of neutron-rich nuclei, and the reach and precision of terrestrial nuclear physics experiments. Nuclear Physics of the Outer Layers of Accreting Neutron StarsFor example, current investigations of the critical reaction rates in X-ray bursts [9,27], studies of key properties of nuclei in the accreted crust [25,26], and nuclear reaction network calculations of accreted crust compositions [22,24,28], all promise to improve the observational constraints on dense matter derived from accreting neutron stars.We begin in section 2 by briefly outlining the neutron star structure. Sections 3 and 4 describe the original composition of the neutron star crust and the accretion process which drives the system from equilibrium. In section 5, we discuss the nuclear burning that can occur on the surface of accreting neutron stars and the nuclei produced during the different possible burning regimes. In actively accreting neutron stars, the ashes of prior surface nuclear burning are compressed to greater depths by newly accreted material. We discuss in section 6 the nuclear interactions involving the ashes that take place as the ambient mass density increases. In section 7, we investigate the impact of interior nuclear interactions on observable neutron star phenomena. We summarize and discuss prospects for future work in section 8.

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Nuclear energy density functional and the nuclear α decay

Cited by 12 publications

References 57 publications

Bayesian modeling of the nuclear equation of state for neutron star tidal deformabilities and GW170817

Bayesian modeling of the nuclear equation of state for neutron star tidal deformabilities and GW170817

Predicting the moment of inertia of pulsar J0737-3039A from Bayesian modeling of the nuclear equation of state

Nuclear physics of the outer layers of accreting neutron stars

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