New mass measurements of 96-98Cd isotopes show the N=50 shell gap strengthens toward 100Sn, tightening constraints on the mass surface in that region.
A Skyrme parametrization from subnuclear to neutron star densitiesPart II. Nuclei far from stabilities
5 Pith papers cite this work, alongside 2,038 external citations. Polarity classification is still indexing.
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Requiring causal stable thermodynamically consistent extensions of neutron-star EOS models to perturbative QCD constrains high-density behavior and disfavors purely nucleonic descriptions for all stable stars.
Causal convolutional neural networks reconstruct neutron star observables for static, Keplerian, and rotating configurations in about 50 milliseconds per equation of state, compared to 30 minutes with traditional RNS calculations.
Simulations show the low-T/|W| instability develops robustly across five nuclear EOS in a rapidly rotating 35 M⊙ progenitor, with dominant GW frequency correlating to PNS compactness and stiffness.
The review describes how SSRPA fixes SRPA pathologies in EDF theory, presents applications to charge-conserving and charge-exchange excitations with experimental comparisons, and discusses impacts on the nuclear equation of state.
citing papers explorer
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Constraining the trend of the $N = 50$ shell gap towards $^{100}$Sn with the masses of $^{96-98}$Cd
New mass measurements of 96-98Cd isotopes show the N=50 shell gap strengthens toward 100Sn, tightening constraints on the mass surface in that region.
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As above, so below: assessing extremeness of the neutron-star equation of state based on the unstable branch
Requiring causal stable thermodynamically consistent extensions of neutron-star EOS models to perturbative QCD constrains high-density behavior and disfavors purely nucleonic descriptions for all stable stars.
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Reconstruction of fast-rotating neutron star observables with the neural network
Causal convolutional neural networks reconstruct neutron star observables for static, Keplerian, and rotating configurations in about 50 milliseconds per equation of state, compared to 30 minutes with traditional RNS calculations.
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Impact of the equation of state on core collapse supernovae I: the low-$T/|W|$ instability
Simulations show the low-T/|W| instability develops robustly across five nuclear EOS in a rapidly rotating 35 M⊙ progenitor, with dominant GW frequency correlating to PNS compactness and stiffness.
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Recent applications of the subtracted second RPA method
The review describes how SSRPA fixes SRPA pathologies in EDF theory, presents applications to charge-conserving and charge-exchange excitations with experimental comparisons, and discusses impacts on the nuclear equation of state.