Abstract
The vector interaction enhanced Bag model (vBag) for dense quark matter extends the commonly used thermodynamic Bag model (tdBag) by incorporating effects of dynamical chiral symmetry breaking (D χ SB) and vector repulsion. Motivated by the suggestion that the stability of strange matter is in tension with chiral symmetry breaking (D χ SB) we examine the parameter space for its stability in the vBag model in this work. Assuming the chiral transition occurs at sufficiently low density, we determine the stability region of strange matter as a function of the effective Bag constant and the vector coupling. As an astrophysical application, we construct contours of maximum mass M max and radius at maximum mass R max in this region of parameter space. We also study the stability of strange stars in the vBag model with maximum mass in the 2 M ⊙ range by computing the spectrum of radial oscillations, and comparing to results from the tdBag model, find some notable differences.
Highlights
It has long been hypothesized [1] that the true ground state of strongly interacting matter in bulk form should comprise of an equal number of up, down and strange quarks, commonly referred to as strange matter [2]
In the vector interaction enhanced Bag model (vBag) model, the vector repulsion is quantified by a coupling parameter Kv which allows the possibility of massive strange stars that are consistent with the 2M observations inferred from compact binaries [7,8]
Having described the EOS for strange stars in the vBag model, we explore radial oscillations, which are of general interest to the dynamics of compact stars [24,25]
Summary
It has long been hypothesized [1] that the true ground state of strongly interacting matter in bulk form should comprise of an equal number of up, down and strange quarks, commonly referred to as strange matter [2]. In the vBag model, the vector repulsion is quantified by a coupling parameter Kv which allows the possibility of massive strange stars (and more generally hybrid stars with quark matter cores [6]) that are consistent with the 2M observations inferred from compact binaries [7,8]. This consistency can be achieved in the simple tdBag model with perturbative αs corrections to the quark pressure, but the applicability of perturbative QCD to the moderate density regime encountered in neutron stars is dubious. We present results for the radial oscillation modes of strange stars in the vBag model model
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