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Experimental Nuclear Masses and the Ground State of Cold Dense Matter
Nuclear Theory · Submitted 4 Oct 1993
abstract compiled · 2026-09-23 · no language-model review
The authors' main claim The most recent experimental data determine the ground state of cold dense matter up to $ \rho \simeq 10^{11}~{\rm g~cm^{-3}} $.
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The abstract, sentence by sentence
We study the consequences of recent progress in the experimental determination of masses of neutron rich nuclei for our knowledge of the ground state of cold dense matter. The most recent experimental data determine the ground state of cold dense matter up to $ \rho \simeq 10^{11}~{\rm g~cm^{-3}} $. The composition and the equation of state of the ground state of matter, in this density interval, are calculated.
background contribution method result interpretation main claim
| # | sentence | role | the authors' own work | states the main conclusion | strength |
|---|---|---|---|---|---|
| s0 | We study the consequences of recent progress in the experimental determination of masses of neutron rich nuclei for our knowledge of the ground state of cold dense matter. | contribution 0.93 | 0.77 | 0.09 | asserted 0.58 |
| s1 | The most recent experimental data determine the ground state of cold dense matter up to $ \rho \simeq 10^{11}~{\rm g~cm^{-3}} $. | result 0.62 | 0.21 | 0.47 | asserted 1.00 |
| s2 | The composition and the equation of state of the ground state of matter, in this density interval, are calculated. | contribution 0.53 | 0.89 | 0.21 | asserted 0.99 |
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The paper
Original abstract
We study the consequences of recent progress in the experimental determination of masses of neutron rich nuclei for our knowledge of the ground state of cold dense matter. The most recent experimental data determine the ground state of cold dense matter up to $ \rho \simeq 10^{11}~{\rm g~cm^{-3}} $. The composition and the equation of state of the ground state of matter, in this density interval, are calculated.
Human review
References
How the literature uses it
23 arXiv papers cite this in 32 sentences
Papers citing it · 17 sentences without a confident label
Uses its method or tool 2 papers
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In this paper we will adopt the unified weak/strong coupling framework of [ref] and construct hybrid EoSs describing three regions: * For nuclear matter (NM) at low densities, up to densities equal to roughly 2 times the saturation density $n_s=0.16$fm$^-3$, we choose various weakly coupled models of nuclear matter that are still plausible given astrophysical constraints, namely: HLPSs [ref] APR [ref] SLy [ref] HLPSi [ref] IUF [ref] ordered here from soft to stiff.
Holographic QCD in the NICER era · Equation of state · 0.92
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In the second section, based on [ref] , we will introduce a matching procedure between the EoS from holography, and a nuclear matter equation of state coming from an effective Skyrme nucleon-nucleon interaction which is expected to work better in the low density regime [ref] .
Holography in Quark-Gluon Plasma and Neutron Stars · Interplay between magnetic field and anisotropy · 0.87
Uses its data or values 5 papers
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It is represented by a relevant low-density part of the SLy4 EOS [ref] .
Approximating neutron-star radii using gravitational-wave only measurements with symbolic regression · Data · 0.98
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The outer crust is thereby taken from Ref. [ref] (Baym-Pethick-Sunderland, BPS) and the inner crust uses the SLy4 model of Ref. [ref] .
Crust (Unified) Tool for Equation-of-state Reconstruction (CUTER) v2 · Application of to existing non-unified EoSs. Example cases. · 0.92
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Therefore, using the results of Refs. [ref] , we model the outer crust as three layers of approximately constant composition[There are small discontinuities in density as we transition between elemental species in these layers, however these discontinuities would smoothen out in a lattice formed by an admixture of elements [ref] .] as summarized in Table [ref].
Warming Nuclear Pasta with Dark Matter: Kinetic and Annihilation Heating of Neutron Star Crusts · Outer Crust · 0.82
Compares with it 2 papers
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It is now easy to show that the neutron drip density is roughly $ρ_ND≈2×10^11$, which is about half of the value obtained in complete calculations [ref] .
Physics of Neutron Star Crusts · Structure of the inner crust · 0.82
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We further compare the sequences of nuclei with those predicted by BPS model, where the binding energies of nuclei obtained with various nuclear models were adopted, i.e., those calculated by * Baym, Pethick, and Sutherland (BPS) [ref] using the nuclear data of Myers and Swiatecki [ref] ; * Haensel, Zdunik, and Dobaczewski [ref] using the nuclear data of Dobaczewski, Flocard, and Treiner (HZD-SkP) [ref] and Myers (HZD-M) [ref] ; * Haensel and Pichon [ref] using the nuclear data of Möller and Nix (HP-MN) [ref] and Aboussir et al. (HP-APDT) [ref] ; * Rüster, Hempel, and Schaffner-Bielich [ref] using the nuclear data of Skyrme (RHS-BSk8) [ref] and RMF models (RHS-TMA) [ref] .
Unified nuclear matter EOSs constrained by the in-medium balance in density-dependent covariant density functionals · Neutron star EOSs in $β$-equilibrium · 0.80
Cites it as background 3 papers
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Inside NSs the matter density increases with radial depth, determining an onion-like equilibrium structure [ref] .
Exploring pulsar glitches with dipolar supersolids · Introduction · 0.84
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For more recent references that employ modern nuclear mass tables see Refs. [ref] .
Impact of the symmetry energy on the outer crust of non-accreting neutron stars · Formalism · 0.88
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While the EOS is understood up to nuclear saturation density $ρ_0 ≈2.7e15$ [ref] , the situation is less clear at super-nuclear densities, with several different models being possible (see, e.g. [ref] ).
Maximum mass and universal relations of rotating relativistic hybrid hadron-quark stars · Introduction · 0.95
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