Rapidly Spinning Compact Stars with Deconfinement Phase Transition

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 that allow purely hadronic uniformly rotating stars with...

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Bibliographic Details
Published in:Astrophysical journal. Letters 2021-02, Vol.907 (2), p.L37
Main Authors: Demircik, Tuna, Ecker, Christian, Järvinen, Matti
Format: Article
Language:English
Subjects:
Equations of state
Neutron stars
Nuclear matter
Phase transitions
Quarks
Stellar rotation
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Summary: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 that 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 ( ) in GW190814 is a neutron star. These stars have central densities that are 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 the largest values for M max / M TOV in cases where the phase transition determines M max , which shifts our fit result to , a value slightly above the Breu–Rezzolla bound inferred from models without phase transition.
ISSN:2041-8205
2041-8213
DOI:10.3847/2041-8213/abd853