Abstract
In this proceedings contribution, we discuss recent developments in the perturbative determination of the Equation of State of dense quark matter, relevant for the microscopic description of neutron star cores. First, we introduce the current state of the art in the problem, both at zero and small temperatures, and then present results from two recent perturbative studies that pave the way towards extending the EoS to higher orders in perturbation theory.
Highlights
The cores of neutron stars contain some of the densest matter in our Universe, second only to the interiors of black holes [1, 2]
With lattice QCD suffering from the infamous Sign Problem [3] and the applicability of Chiral Effective Theory (CET) extending only up to roughly the nuclear matter saturation density [4], there is an urgent need to find complementary methods for tackling strongly coupled matter at the the highest densities reached within the stars
We describe recent efforts to approach the problem of quark matter using insights gained from the limit of very high densities, where a weak coupling approach is guaranteed to be valid due to the asymptotic freedom of the underlying theory
Summary
The cores of neutron stars contain some of the densest matter in our Universe, second only to the interiors of black holes [1, 2]. With lattice QCD suffering from the infamous Sign Problem [3] and the applicability of Chiral Effective Theory (CET) extending only up to roughly the nuclear matter saturation density [4], there is an urgent need to find complementary methods for tackling strongly coupled matter at the the highest densities reached within the stars This has motivated attempts to approach the problem using methods ranging from the Functional Renormalization Group to phenomenological models and the holographic duality [5,6,7,8,9,10], but they all come with their own systematic uncertainties and limitations.
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