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Emergence of Calabi-Yau manifolds in high-precision black-hole scattering. [PDF]
NatureDriesse M +7 more
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Dynamical Signatures of <i>Thermotoga maritima</i> Maltose-Binding Proteins Affected by Ligand Binding. [PDF]
ACS OmegaShukla S +6 more
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Cu<sub>14</sub>H<sub>12</sub>(P<i><sup>t</sup></i>Bu<sub>3</sub>)<sub>6</sub>Cl<sub>2</sub>-The Expanse of Stryker's Reagent. [PDF]
MoleculesStrienz M +3 more
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Kilonova simulations: connecting observations with the underlying physics. [PDF]
Philos Trans A Math Phys Eng SciCollins C, Shingles L, Vijayan V.
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Physical Review Letters, 1993
We calculate properties of neutron star matter at subnuclear densities using an improved nuclear Hamiltonian. Nuclei disappear and the matter becomes uniform at a density of about 0.6n(s), where n(s) of about 0.16/cu fm is the saturation density of nuclear matter. As a consequence, the mass of matter in the crusts of neutron stars is only about half as
, Lorenz, , Ravenhall, , Pethick
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We calculate properties of neutron star matter at subnuclear densities using an improved nuclear Hamiltonian. Nuclei disappear and the matter becomes uniform at a density of about 0.6n(s), where n(s) of about 0.16/cu fm is the saturation density of nuclear matter. As a consequence, the mass of matter in the crusts of neutron stars is only about half as
, Lorenz, , Ravenhall, , Pethick
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Nuclear Physics A, 1971
Abstract The matter in neutron stars is essentially in its ground state and ranges in density up to and beyond 3 × 10 14 g/cm 3 , the density of nuclear matter. Here we determine the constitution of the ground state of matter and its equation of state in the regime from 4.3 × 10 11 g/cm 3 where free neutrons begin to “drip” out of the nuclei, up ...
GORDON BAYM +2 more
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Abstract The matter in neutron stars is essentially in its ground state and ranges in density up to and beyond 3 × 10 14 g/cm 3 , the density of nuclear matter. Here we determine the constitution of the ground state of matter and its equation of state in the regime from 4.3 × 10 11 g/cm 3 where free neutrons begin to “drip” out of the nuclei, up ...
GORDON BAYM +2 more
openaire +1 more source