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- W3129075185 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 $2.9, mathrm{M}_odot$, 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. We find largest values for $M_{mathrm{max}}/M_{mathrm{TOV}}$ in cases where the phase transition determines $M_{mathrm{max}}$, which shifts our fit result to $M_{mathrm{max}}/M_{mathrm{TOV}} = 1.227^{+0.031}_{-0.016}$, a value slightly above the Breu-Rezzolla bound $1.203^{+0.022}_{-0.022}$ inferred from models without phase transition." @default.
- W3129075185 created "2021-02-15" @default.
- W3129075185 creator A5034855787 @default.
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- W3129075185 date "2021-01-29" @default.
- W3129075185 modified "2023-10-17" @default.
- W3129075185 title "Rapidly Spinning Compact Stars with Deconfinement Phase Transition" @default.
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- W3129075185 doi "https://doi.org/10.3847/2041-8213/abd853" @default.
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