Constraints from compact star observations on non-Newtonian gravity in strange stars based on a density dependent quark mass model

Abstract

Using a density dependent quark mass (QMDD) model for strange quark matter, we investigate the effects of non-Newtonian gravity on the properties of strange stars and constrain the parameters of the QMDD model by employing the mass of PSR J0740+6620 and the tidal deformability of GW170817. We find that for QMDD model these mass and tidal deformability observations would rule out the existenceof str ange stars if non-Newtonian gravity effects are ignored. For the current quark masses of $m_{u0}=2.16$ MeV, $m_{d0}=4.67$ MeV, and $m_{s0}=93$ MeV, we find that a strange star can exist for values of the non-Newtonian gravity parameter $g^2/{\mu }^2$ in the range of 4.58 GeV${}^{-2}\le g^2/{\mu }^2\le$ 9.32 GeV${}^{-2}$, and that the parameters $D$ and $C$ of the QMDD modelare restricted to 158.3 MeV$\le D^{1/2}\le$ 181.2 MeV and $-0.65\le C\le -0.12$. It is found that the largest possible maximum mass of a strange star obtained with the QMDD model is $2.42M_{\odot }$, and that the secondary componentof GW190814 with a mass of 2.59_{-0.09}^{+0.08}\, M_{\dot} could not be a static strange star. We also find that forthe mass and radius of PSR J0030+0451 given by Riley et al. through the analysis of observational data of NICER, there exists a very tiny allowed parameter space for which strange stars computed for the QMDD model agree with the observations of PSR J0740+6620, GW17 0817 and PSR J0030+0451 simultaneously. However, for the mass and radius given by Miller et al., no such parameter space exist.

arXiv comment8 pages, 4 figures, accepted by Phys. Rev. D

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• Strange stars with a mirror-dark-matter core confronting with the observations of compact stars
• Vetting quark-star models with gravitational waves in the hierarchical Bayesian framework
• Confronting recent light compact star observations with color-flavor locked quark matter
• On the Cooling of Compact Stars in Light of the HESS J1731-347 Remnant