First measurement of ^4_ΛHe yields in 3 GeV Au+Au collisions shows consistency with ^4_ΛH yields and JAM coalescence model while thermal model overpredicts absolute yields.
Hyperon Puzzle: Hints from Quantum Monte Carlo Calculations
5 Pith papers cite this work. Polarity classification is still indexing.
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abstract
The onset of hyperons in the core of neutron stars and the consequent softening of the equation of state have been questioned for a long time. Controversial theoretical predictions and recent astrophysical observations of neutron stars are the grounds for the so-called hyperon puzzle. We calculate the equation of state and the neutron star mass-radius relation of an infinite systems of neutrons and $\Lambda$ particles by using the auxiliary field diffusion Monte Carlo algorithm. We find that the three-body hyperon-nucleon interaction plays a fundamental role in the softening of the equation of state and for the consequent reduction of the predicted maximum mass. We have considered two different models of three-body force that successfully describe the binding energy of medium mass hypernuclei. Our results indicate that they give dramatically different results on the maximum mass of neutron stars, not necessarily incompatible with the recent observation of very massive neutron stars. We conclude that stronger constraints on the hyperon-neutron force are necessary in order to properly assess the role of hyperons in neutron stars.
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Bayesian analysis of astrophysical and laboratory data favors the two-families scenario of coexisting hadronic and strange quark stars over the one-family scenario.
Hypertriton yields and Lambda ratios increase at lower collision energies but remain a factor of two below thermal models, while the double ratio to triton production stays constant at 0.4, pointing to intrinsically lower coalescence probability.
Including hyperons reduces maximum neutron-star mass by 0.05-0.10 solar masses and increases radius at 1.4 solar masses by 0.5-0.8 km across all models while keeping every equation of state consistent with the 2-solar-mass limit.
The IdylliQ model uses quark saturation to generate stiff equations of state and effective baryon repulsions that mitigate hyperon softening in neutron star matter.
citing papers explorer
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Hyper-Nuclei $^4_{\Lambda}\hbox{He}$ Production in $\sqrt{s_{\rm{NN}}}$ = 3 GeV Au+Au collisions at RHIC
First measurement of ^4_ΛHe yields in 3 GeV Au+Au collisions shows consistency with ^4_ΛH yields and JAM coalescence model while thermal model overpredicts absolute yields.
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Is the coexistence of strange quark stars and hadronic stars favored by astrophysical data? A Bayesian analysis
Bayesian analysis of astrophysical and laboratory data favors the two-families scenario of coexisting hadronic and strange quark stars over the one-family scenario.
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Collision Energy Dependence of Hypertriton Production in Au+Au Collisions at RHIC
Hypertriton yields and Lambda ratios increase at lower collision energies but remain a factor of two below thermal models, while the double ratio to triton production stays constant at 0.4, pointing to intrinsically lower coalescence probability.
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Hyperonic equation of state for neutron stars: A systematic Bayesian comparison of density-dependent and non-linear relativistic mean-field models
Including hyperons reduces maximum neutron-star mass by 0.05-0.10 solar masses and increases radius at 1.4 solar masses by 0.5-0.8 km across all models while keeping every equation of state consistent with the 2-solar-mass limit.
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A quarkyonic matter model
The IdylliQ model uses quark saturation to generate stiff equations of state and effective baryon repulsions that mitigate hyperon softening in neutron star matter.