However, for the mass and radius given by Miller et al., no such parameter space exist. 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 J 0740 + 6620, GW170817 and PSR J 0030 + 0451 simultaneously. We also find that for the mass and radius of PSR J 0030 + 0451 given by Riley et al. It is found that the largest possible maximum mass of a strange star obtained with the QMDD model is 2.42 M ⊙ and that the secondary component of GW190814 with a mass of 2.59 − 0.09 + 0.08 M ⊙ could not be a static strange star.
For the current quark masses of m u 0 = 2.16 MeV, m d 0 = 4.67 MeV, and m s 0 = 93 MeV, we find that a strange star can exist for values of the non-Newtonian gravity parameter g 2 / μ 2 in the range of 4.58 GeV − 2 ≤ g 2 / μ 2 ≤ 9.32 GeV − 2, and that the parameters D and C of the QMDD model are restricted to 158.3 MeV ≤ D 1 / 2 ≤ 181.2 MeV and − 0.65 ≤ C ≤ − 0.12. We find that for the QMDD model these mass and tidal deformability observations would rule out the existence of strange stars if non-Newtonian gravity effects are ignored. 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 J 0740 + 6620 and the tidal deformability of GW170817.
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