Dispersive optical model analyses of 40Ca to 208Pb nuclei show neutron skin thickness rising stronger than linearly with asymmetry, consistent with GFMC He results and drip-line expectations.
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Short-range correlations soften neutron-star equations of state with quadratic vector self-interactions but stiffen them with an added fourth-order term, producing corresponding shifts in maximum masses that persist when a dark-matter fluid is included.
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Dispersive-optical-model analysis of the asymmetry dependence of neutron skins
Dispersive optical model analyses of 40Ca to 208Pb nuclei show neutron skin thickness rising stronger than linearly with asymmetry, consistent with GFMC He results and drip-line expectations.
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Effects of short-range correlations at high densities on neutron stars with and without DM content: role of the repulsive self-interaction
Short-range correlations soften neutron-star equations of state with quadratic vector self-interactions but stiffen them with an added fourth-order term, producing corresponding shifts in maximum masses that persist when a dark-matter fluid is included.