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Long Range Plan: Dense matter theory for heavy-ion collisions and neutron stars
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Since the release of the 2015 Long Range Plan in Nuclear Physics, major events have occurred that reshaped our understanding of quantum chromodynamics (QCD) and nuclear matter at large densities, in and out of equilibrium. The US nuclear community has an opportunity to capitalize on advances in astrophysical observations and nuclear experiments and engage in an interdisciplinary effort in the theory of dense baryonic matter that connects low- and high-energy nuclear physics, astrophysics, gravitational waves physics, and data science
Forward citations
Cited by 7 Pith papers
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Space-time regions of high baryon density and baryon stopping in heavy-ion collisions
3FD hydrodynamics predicts larger and longer-lived regions of dense baryon matter in Au+Au collisions at 3–19.6 GeV than JAM transport, with V4(3n0) decreasing monotonically with energy.
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Locating the QCD critical point with neutron-star observations
Bayesian analysis of a hybrid holographic EOS with neutron-star constraints locates the QCD critical endpoint at μ≈626 MeV and T≈119 MeV and predicts a strong first-order deconfinement transition at zero temperature.
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Quantum computation of hadron scattering in a lattice gauge theory
On a trapped-ion quantum computer, the authors prepared multiple meson wave packets and simulated their early-time collisions in a 1+1D Z2 lattice gauge theory.
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A Critical Point on the Hairy Black Hole Phase Boundary in the Improved Holographic Einstein-Maxwell-Dilaton Theory
In the improved holographic EMD model, two hairy black hole phases are separated by a U-shaped boundary whose lower branch is first-order and upper branch third-order, meeting at (mu_B,T)=(765.51,86.54) MeV.
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The equation of state and surface tension of QCD in the first order phase transition region
A parametrized order-parameter model yields the equation of state, spinodal boundaries, and surface tension for the first-order QCD phase transition.
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An Effective Upper Bound on the Pressure-to-Energy Density Ratio in Neutron Stars
Using a fitted effective correction in their IPAD-TOV framework, the authors obtain X≲0.385, a looser bound than their earlier 0.374, plus an empirical compactness scaling fit to 284 EOSs.
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The equation of state for neutron stars
A textbook-style review of the neutron-star equation of state covering the models, experimental and observational constraints, and open questions, with no new result claimed or derived.
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