Delineating the properties of matter in cold, dense QCD
arXiv:1904.05080 · doi:10.1063/1.5117813
Abstract
The properties of dense QCD matter are delineated through the construction of equations of state which should be consistent with QCD calculations in the low and high density limits, nuclear laboratory experiments, and the neutron star observations. These constraints, together with the causality condition of the sound velocity, are used to develop the picture of hadron-quark continuity in which hadronic matter continuously transforms into quark matter (modulo small 1st order phase transitions). For hadronic matter (at baryon density nB > ~2n0 with n0 ~ 0.16 fm^(-3) being the nuclear saturation density) we use equations of state by Togashi et al. based on microscopic variational many-body calculations, and for quark matter (nB > ~5n0) we construct equations of state using a schematic quark model (with strangeness) whose interactions are motivated by the hadron phenomenology. The region between hadronic and quark matters (~2n0 < nB < ~5n0), which is most difficult to calculate, is treated by highly constrained interpolation between nuclear and quark matter equations of state. The resultant unified equation of state at zero temperature and beta-equilibrium, which we call Quark-Hadron-Crossover (QHC18 and QHC19), is consistent with the measured properties of neutron stars and in addition gives us microscopic insights into the properties of dense QCD matter. In particular to ~10n0 the gluons can remain as non-perturbative as in vacuum and the strangeness can be as abundant as up- and down-quarks at the core of two-solar mass neutron stars. Within our modeling the maximum mass is found less than ~2.35 times solar mass and the baryon density at the core ranges in ~5-8n0.
18 pages 11 figures, AIP Proceedings of the Xiamen-CUSTIPEN Workshop on the EOS of Dense Neutron-Rich Matter in the Era of Gravitational Wave Astronomy, Jan. 3-7, Xiamen, China; v2 references are added
References in corpus (19)
- Shapiro delay measurement of a two solar mass neutron star
- A Massive Pulsar in a Compact Relativistic Binary
- Color superconductivity in dense quark matter
- Neutron Star Observations: Prognosis for Equation of State Constraints
- Tidal Love numbers of neutron stars
- Swope Supernova Survey 2017a (SSS17a), the Optical Counterpart to a Gravitational Wave Source
- Using gravitational-wave observations and quasi-universal relations to constrain the maximum mass of neutron stars
- Cold Quark Matter
- A new quark-hadron hybrid equation of state for astrophysics - I. High-mass twin compact stars
- Symmetry energy from elliptic flow in 197Au + 197Au
- New Critical Point Induced by the Axial Anomaly in Dense QCD
- Nuclear equation of state for core-collapse supernova simulations with realistic nuclear forces
- New Neutron Star Equation of State with Quark-Hadron Crossover
- Baryons and the phase diagram for a large number of colors and flavors
- Pions in Large- Quantum Chromodynamics
- Solving two-dimensional large-N QCD with a nonzero density of baryons and arbitrary quark mass
- Effective repulsion in dense quark matter from non-perturbative gluon exchange
- Finite-density gauge correlation functions in QC2D
- Number of the QCD critical points with neutral color superconductivity
Cited by in corpus (6)
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- Stiffening of matter in quark-hadron continuity
- The slope, the hill, the drop, and the swoosh: Learning about the nuclear matter equation of state from the binary Love relations
- Modern nuclear and astrophysical constraints of dense matter in a renormalized chiral approach
- Impact of Multiple Phase Transitions in Dense QCD on Compact Stars
- Stiffening of matter in quark-hadron continuity: a mini-review