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Neutron Stars Mass-Radius relations analysis in the Quintessence scenario
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In this paper, we explore the effects of General Relativity modification on the Mass-Radius relations of Neutron Stars induced by the presence of the Quintessence field. We consider, in particular, the Kiselev model, according to which the Quintessence field, being present in the entire Universe, might also be present around massive objects. Considering the Equation of State (EoS) for Baryonic matter BSk22 derived by A. Y. Potekhin et al., we infer the upper limit for NS masses in the presence of Quintessence. The presence of Quintessence generates a peculiar effect for which the Mass-Radius relation is unvaried and therefore the presence of Quintessence is indistinguishable from ordinary matter, at least for the Kiselev model studied in this paper.
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Quintessence-Chameleon transitions in anisotropic Kiselev model of neutron stars
A chameleon-Kiselev neutron star model claims scalar-driven pressure anisotropies, a 1.75 solar mass maximum, and an 86% tidal deformability suppression, but headline numbers contradict each other across the paper.
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