Abstract
The structure of neutron stars is investigated in the context of a scalar-tensor theory of gravity with variable Brans-Dicke parameter ω(Φ). Neutron star models are constructed using the Pandharipande (hyperon) equation of state and an equation of state that maximizes the mass for various values of the variability parameter α= 2ω'(Φ)/[3+2ω(Φ)] 2 . It is shown that the neutron stars are more compact and less massive than their counterparts in general relativity and standard Brans-Dicke theory
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