  A Newtonian-like theory inspired by the Brans-Dicke gravitational Lagrangian
has been recently proposed. For static configurations the gravitational
coupling acquires an intrinsic spatial dependence within the matter
distribution. Therefore, the interior of astrophysical configurations may
provide a testable environment for this approach as long as no screening
mechanism is evoked. In this work we focus on the stellar hydrostatic
equilibrium structure in such varying $G$ scenario. A modified Lane-Emden
equation is presented and its solutions for various values of the polytropic
index are discussed. The role played by the theory parameter $\omega$, the
analogue of the Brans-Dicke parameter, on the physical properties of stars is
discussed.
