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2020

Rapidly Spinning Compact Stars with Deconfinement Phase Transition

Demircik, Tuna, Ecker, Christian, Järvinen, Matti

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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 $2.9\, \mathrm{M}_\odot$, and are therefore compatible with the interpretation that the secondary component ($2.59^{+0.08}_{-0.09}\, \mathrm{M}_\odot$) 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 $M_{\mathrm{TOV}}$ ($M_{\mathrm{max}}$) is either determined by the secular instability or a phase transition induced collapse.

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