From neutron skins and neutron matter to the neutron star crust

Newton, William; Preston, Rebecca; Balliet, Lauren; Ross, Michael G.

doi:10.48550/arxiv.2111.07969

Cited by 4 publications

(15 citation statements)

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“…Our inferences of crust properties are the first to extract constraints from PREX from direct EDF calculations of the neutron skin of lead and combine them with astrophysical data using unified EOSs with high density polytropes. Our results are consistent with our previous work focusing solely on the crust EOS [76,77] and the similar calculations of [47,74,75]. Our results for the ratio of the thickness and mass of pasta to that of the crust incorporating PREX with NICER+LV is ∆R c /∆R p = 0.172 +0.025 −0.124 and ∆M c /∆M p = 0.51 +0.08 −0.36 , compared with ∆R c /∆R p = 0.19 +0.05 −0.07 and ∆M c /∆M p = 0.57 +0.10 −0.17 from PREX data alone [77], and ∆R c /∆R p = 0.128 +0.047 −0.047 and ∆M c /∆M p = 0.49 +0.14 −0.14 from an analysis without PREX data, but incorporating information on the pure neutron matter EOS [75].…”

Section: Discussionsupporting

confidence: 93%

“…Neither astrophysical data nor PREX data narrow the uncertainty in the crust and pasta thicknesses, mass or moments of inertia; indeed, the uncertainty appears to increase significantly with the PREX data, an artifact of the increased likelihood of no pasta causing a second peak in the distribution [77]. Thus currently data is giving information about the most likely value, but not increasing the precision of the prediction.…”

Section: Resultsmentioning

confidence: 89%

“…Not all combinations of parameters produce viable crust models due to instabilities in the PNM EOS at low crust densities, so the symmetry energy space naturally gets filtered by this physical requirement. See [76,77] and Fig. 2 for the resulting parameter space for our priors.…”

Section: Resultsmentioning

confidence: 99%

“…Explorations of the space of neutron star crust EOSs are not as developed as those of the core EOS. There exists only two attempts to systematically generate of crust model ensembles, using meta-models [74,75,48] and using an extended Skyrme EDF [76,77].…”

Section: Introductionmentioning

confidence: 99%

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Ensembles of unified crust and core equations of state in a nuclear-multimessenger astrophysics environment

Newton,

Balliet,

Budimir

et al. 2021

Preprint

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We present an ensemble of unified neutron star crust and core equations of state, constructed using an extended Skyrme energy density functional through the crust and outer core, and appended by two piecewise polytropes at higher densities. The equations of state are parameterized by the first three coefficients in the density expansion of the symmetry energy J, L and Ksym, the moment of inertia of a 1.338 M star I1.338 and the maximum neutron star mass Mmax. We construct an ensemble with uniform priors on all five parameters, and then apply data filters to the ensemble to explore the effect of combining neutron skin data from PREX with astrophysical measurements of radii and tidal deformabilities from NICER and LIGO/VIRGO. Neutron skins are calculated directly using the EDFs. We demonstrate that both the nuclear data and astrophysical data play a role in constraining crust properties such as the mass, thickness and moment of inertia of the crust and the nuclear pasta layers therein, and that astrophysical data better constrains Ksym than PREX data.

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Section: Discussionsupporting

confidence: 93%

Section: Resultsmentioning

confidence: 89%

Section: Resultsmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

See 2 more Smart Citations

Ensembles of unified crust and core equations of state in a nuclear-multimessenger astrophysics environment

Newton,

Balliet,

Budimir

et al. 2021

Preprint

Self Cite

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“…Although there exists no direct and robust observational evidence of nuclear pasta, various tantalizing observations indicate its existence [23][24][25]. Numerous theoretical attempts based on molecular dynamics simulations [22,26,27], compressible liquid-drop models [28,29], Thomas-Fermi method [6,30,31] and nuclear density functional theory [32] point towards the possibility of the pasta structures near the crust-core transition density. The amount of these structures in the inner crust plays pivotal role in the explanation of various neutron star mechanisms such as crust cooling [25,33], spin period [24], quasiperiodic oscillation in giant flares [34], transport [35], shattering of the crust [36] etc.…”

Section: Introductionmentioning

confidence: 99%

Crustal properties of a neutron star within an effective relativistic mean-field model

et al. 2022

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We study the properties of pasta structures and their influence on the neutron star observables employing the effective relativistic mean-field theory (E-RMF). The compressible liquid drop model is used to incorporate the finite size effects, considering the possibility of non-spherical structures in the inner crust. The unified equation of state are constructed for several E-RMF parameters to study various properties such as pasta mass and thickness in the neutron star's crust. The majority of the pasta properties are sensitive to the symmetry energy in the subsaturation density region. Using the results from Monte Carlo simulations, we estimate the shear modulus of the crust in context of quasiperiodic oscillations from soft gamma-ray repeaters and calculate the frequency of fundamental torsional oscillation mode in the inner crust. Global properties of the neutron star such as mass-radius profile, the moment of inertia, crustal mass, crustal thickness and fractional crustal moment of inertia are worked out. The results are consistent with various observational and theoretical constraints.

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Investigating dark matter-admixed neutron stars with NITR equation of state in light of PSR J0952-0607

Routaray,

Mohanty,

Das

et al. 2023

J. Cosmol. Astropart. Phys.

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The fastest and heaviest pulsar, PSR J0952-0607, with a mass of M = 2.35±0.17 M ⊙, has recently been discovered in the disk of the Milky Way Galaxy. In response to this discovery, a new RMF model, 'NITR' has been developed. The NITR model's naturalness has been confirmed by assessing its validity for various finite nuclei and nuclear matter properties, including incompressibility, symmetry energy, and slope parameter values of 225.11, 31.69, and 43.86 MeV, respectively. These values satisfy the empirical/experimental limits currently available. The maximum mass and canonical radius of a neutron star (NS) calculated using the NITR model parameters are 2.355 M ⊙ and 13.13 km, respectively, which fall within the range of PSR J0952-0607 and the latest NICER limit. This study aims to test the consistency of the NITR model by applying it to various systems. As a result, its validity is extensively calibrated, and all the nuclear matter and NS properties of the NITR model are compared with two established models such as IOPB-I and FSUGarnet. In addition, the NITR model equation of state (EOS) is employed to obtain the properties of a dark matter admixed NS (DMANS) using two approaches (I) single-fluid and (II) two-fluid approaches. In both cases, the EOS becomes softer due to DM interactions, which reduces various macroscopic properties such as maximum mass, radius, tidal deformability, etc. The various observational data such as NICER and HESS are used to constrain the amount of DM in both cases. Moreover, we discuss the impact of dark matter (DM) on the nonradial f-mode frequency of the NS in a single fluid case only and try to constrain the amount of DM using different theoretical limits available in the literature.

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From neutron skins and neutron matter to the neutron star crust

Cited by 4 publications

References 0 publications

Ensembles of unified crust and core equations of state in a nuclear-multimessenger astrophysics environment

Ensembles of unified crust and core equations of state in a nuclear-multimessenger astrophysics environment

Crustal properties of a neutron star within an effective relativistic mean-field model

Investigating dark matter-admixed neutron stars with NITR equation of state in light of PSR J0952-0607

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