A Bayesian combination of eight M-R posteriors for PSR J0030+0451 yields M = 1.46^{+0.09}_{-0.08} M_⊙, R = 12.69^{+0.64}_{-0.55} km while marginalizing over unknown model systematics.
Generic conditions for stable hybrid stars.Phys
5 Pith papers cite this work, alongside 401 external citations. Polarity classification is still indexing.
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Relaxing the onset assumption for stiff high-density matter raises the theoretical maximum neutron star mass to 4 solar masses or higher.
Hybrid star models with constant sound speed quark matter match NICER data for PSR J0740+6620 and PSR J0030+0451 only when the energy density discontinuity at the phase transition is small and the quark sound speed is relatively high.
Review summarizing the role of dense-matter equation of state, weak interactions, and r-process nucleosynthesis in binary neutron star mergers and their multimessenger observables.
citing papers explorer
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Combining the Mass--Radius Posteriors of J0030+0451 Allowing for Unknown Model Systematics
A Bayesian combination of eight M-R posteriors for PSR J0030+0451 yields M = 1.46^{+0.09}_{-0.08} M_⊙, R = 12.69^{+0.64}_{-0.55} km while marginalizing over unknown model systematics.
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Revisiting the Rhoades-Ruffini bound
Relaxing the onset assumption for stiff high-density matter raises the theoretical maximum neutron star mass to 4 solar masses or higher.
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Can a hybrid star with constant sound speed parametrization explain the new NICER mass-radius measurements ?
Hybrid star models with constant sound speed quark matter match NICER data for PSR J0740+6620 and PSR J0030+0451 only when the energy density discontinuity at the phase transition is small and the quark sound speed is relatively high.
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Nuclear Physics of Binary Neutron Star Mergers
Review summarizing the role of dense-matter equation of state, weak interactions, and r-process nucleosynthesis in binary neutron star mergers and their multimessenger observables.
- On the Possibility of a Strong First-Order Phase Transition in Neutron Stars