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Gravitational-Wave Constraints on the Neutron-Star-Matter Equation of State.
TLDR
It is concluded that the maximal radius of a 1.4-solar-mass neutron star is 13.6 km, and that the smallest allowed tidal deformability of a similar-mass star is Λ(1.4  M_{⊙})=120.4%.
Cold quark matter
We perform an O({alpha}{sub s}{sup 2}) perturbative calculation of the equation of state of cold but dense QCD matter with two massless and one massive quark flavor, finding that perturbation theory
Evidence for quark-matter cores in massive neutron stars
The theory governing the strong nuclear force—quantum chromodynamics—predicts that at sufficiently high energy densities, hadronic nuclear matter undergoes a deconfinement transition to a new phase
Basics of Thermal Field Theory
These lecture notes, suitable for a two-semester introductory course or self-study, offer an elementary and self-contained exposition of the basic tools and concepts that are encountered in practical
Constraining Neutron Star Matter with Quantum Chromodynamics
In recent years, there have been several successful attempts to constrain the equation of state of neutron star matter using input from low-energy nuclear physics and observational data. We
Spinning Dragging Strings
We use the AdS/CFT correspondence to compute the drag force experienced by a heavy quark moving through a = 4 SU(N) super Yang-Mills plasma at nonzero temperature and R-charge chemical potential and
QCD and strongly coupled gauge theories: challenges and perspectives
TLDR
In the course of the work, a perspective on the many research streams which flow into and out of QCD is offered, as well as a vision for future developments.
Interacting quark matter equation of state for compact stars
Lattice QCD studies of thermodynamics of hot quark-gluon plasma (QGP) demonstrate the importance of accounting for the interactions of quarks and gluons, if one wants to investigate the phase
Pressure of QCD at finite temperatures and chemical potentials
We compute the perturbative expansion of the pressure of hot QCD to order g(6)ln g in the presence of finite quark chemical potentials. In this process we evaluate all two- and three-loop vacuum
Neutron star structure from QCD
Abstract.In this review article, we argue that our current understanding of the thermodynamic properties of cold QCD matter, originating from first principles calculations at high and low densities,
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