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Probing neutron-star matter in the lab: similarities and differences between binary mergers and heavy-ion collisions
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abstract
Binary neutron-star mergers and heavy-ion collisions are related through the properties of the hot and dense nuclear matter formed during these extreme events. In particular, low-energy heavy-ion collisions offer exciting prospects to recreate such {extreme} conditions in the laboratory. However, it remains unexplored to what degree those collisions can actually reproduce hot and dense matter formed in binary neutron star mergers. As a way to understand similarities and differences between these systems, we {discuss their geometry and }perform a direct numerical comparison of the thermodynamic conditions probed in both collisions. To enable a direct comparison, we employ a finite-temperature equation of state able to describe the entire high-energy phase diagram of Quantum Chromodynamics. Putting side by side the evolution of both systems, we find that laboratory heavy-ion collisions at the energy range of $E_{\mathrm{lab}}=0.4 - 0.6\ A$ MeV probe (thermodynamic) states of matter that are very similar to those created in binary neutron-star mergers. These results can inform future low-energy heavy-ion collisions probing this regime.
Forward citations
Cited by 6 Pith papers
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In UrQMD simulations of Au+Au at SIS18/SIS100 energies, the final midrapidity elliptic flow is generated late by the mean-field potential during the breakup of a matter bridge, not by early squeeze-out or spectator shadowing.
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Post-Merger Gravitational-Wave Uncertainties of Binary Neutron Stars under Multi-Messenger EOS Constraints
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Directed and elliptic flow of light nuclei and hypernuclei in Au+Au collisions at $\sqrt{s_\mathrm{NN}}=3$ GeV: Coalescence vs. Statistical Fragmentation
In UrQMD, both coalescence and statistical fragmentation give mass-number scaling of directed flow for (hyper)nuclei at 3 GeV that matches STAR, while elliptic flow scaling is not seen in the data.
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Building Neutron Stars with the MUSES Calculation Engine
A new open-source calculation engine produces crust-to-core neutron star equations of state and shows that smooth matching choices change predicted radii and masses by several percent.
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Simultaneous description of high density QCD matter in heavy ion collisions and neutron star observations
An equation of state selected to match neutron star mass-radius data also describes HADES heavy-ion observables when implemented with momentum-dependent potentials in UrQMD.
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A review of transport-model constraints on the nuclear equation of state from flow of protons, light clusters, and hypernuclei, concluding that soft momentum-dependent potentials fit few-GeV data best.
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