Abstract
It is demonstrated how in the absence of solutions for QCD under conditions deep inside compact stars an equation of state can be obtained within a model that is built on the basic symmetries of the QCD Lagrangian, in particular chiral symmetry and color symmetry. While in the vacuum the chiral symmetry is spontaneously broken, it gets restored at high densities. Color symmetry, however, gets broken simultaneously by the formation of colorful diquark condensates. It is shown that a strong diquark condensate in cold dense quark matter is essential for supporting the possibility that such states could exist in the recently observed pulsars with masses of 2 M ʘ .
Highlights
It is demonstrated how in the absence of solutions for quantum chromodynamics (QCD) under conditions deep inside compact stars an equation of state can be obtained within a model that is built on the basic symmetries of the QCD Lagrangian, in particular chiral symmetry and color symmetry
I will elucidate this statement on the example of the QCD phase diagram and the question for quark matter in compact stars
For the application of the above described low-energy QCD model to study the composition of compact star interiors one has to embody the constraints of electric neutrality and β−equilibrium to the thermodynamic potential and use the resulting T = 0 equation of state (EoS) for the pressure p(μ) = Ω(T = 0, {μ}) from which all other thermodynamic functions can be derived which are required to solve the Tolman-Oppenheimer-Volkoff equations of compact star stability
Summary
It is demonstrated how in the absence of solutions for QCD under conditions deep inside compact stars an equation of state can be obtained within a model that is built on the basic symmetries of the QCD Lagrangian, in particular chiral symmetry and color symmetry.
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