Rapidly Spinning Compact Stars with Deconfinement Phase Transition

Tuna Demircik; Christian Ecker; Matti Järvinen

doi:10.3847/2041-8213/abd853

paper

Rapidly Spinning Compact Stars with Deconfinement Phase Transition

arXiv:2009.10731 · doi:10.3847/2041-8213/abd853

Abstract

We study rapidly spinning compact stars with equations of state featuring a first order phase transition between strongly coupled nuclear matter and deconfined quark matter by employing the gauge/gravity duality. We consider a family of models, which allow purely hadronic uniformly rotating stars with masses up to approximately $2.9 M_{⊙}$ , and are therefore compatible with the interpretation that the secondary component ( $2.5 9_{- 0.09}^{+ 0.08} M_{⊙}$ ) in GW190814 is a neutron star. These stars have central densities several times the nuclear saturation density so that strong coupling and non-perturbative effects become crucial. We construct models where the maximal mass of static (rotating) stars $M_{TOV}$ ( $M_{max}$ ) is either determined by the secular instability or a phase transition induced collapse. We find largest values for $M_{max} / M_{TOV}$ in cases where the phase transition determines $M_{max}$ , which shifts our fit result to $M_{max} / M_{TOV} = 1.22 7_{- 0.016}^{+ 0.031}$ , a value slightly above the Breu-Rezzolla bound $1.20 3_{- 0.022}^{+ 0.022}$ inferred from models without phase transition.

7 pages, 5 figures, comments welcome

Rapidly Spinning Compact Stars with Deconfinement Phase Transition

Abstract

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