Constraints on the maximum mass of neutron stars with a quark core from GW170817 and NICER PSR J0030+0451 data

Abstract

We perform a Bayesian analysis of the maximum mass $M_{\mathrm{TOV}}$ of neutron stars with a quark core, incorporating the observational data from tidal deformability of the GW170817 binary neutron star merger as detected by LIGO/Virgo and the mass and radius of PSR J0030+0451 as detected by \nicer. The analysis is performed under the assumption that the hadron-quark phase transition is of first order, where the low-density hadronic matter described in a unified manner by the soft QMF or the stiff DD2 equation of state (EOS) transforms into a high-density phase of quark matter modeled by the generic "Constant-sound-speed" (CSS) parameterization. The mass distribution measured for the $2.14{\mathrm{M}}_{\odot }$ pulsar, MSP J0740+6620, is used as the lower limit on $M_{\mathrm{TOV}}$. We find the most probable values of the hybrid star maximum mass are $M_{\mathrm{TOV}}=2.36_{-0.26}^{+0.49}{\mathrm{M}}_{\odot }$ ($2.39_{-0.28}^{+0.47}{\mathrm{M}}_{\odot }$) for QMF (DD2), with an absolute upper bound around $2.85{\mathrm{M}}_{\odot }$, to the $90\%$ posterior credible level. Such results appear robust with respect to the uncertainties in the hadronic EOS. We also discuss astrophysical implications of this result, especially on the post-merger product of GW170817, short gamma-ray bursts, and other likely binary neutron star mergers.

13 pages, 8 figures, 2 tables, to appear in ApJ

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