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In this work we analyze hydrostatic equilibrium configurations of neutronstars in a non-minimal geometry-matter coupling (GMC) theory of gravity. Webegin with the derivation of the hydrostatic equilibrium equations for the$f(R,L) $ gravity theory, where $R$ and $L$ are the Ricci scalar and Lagrangianof matter, respectively. We assume $f(R,L)=R/2+[1+\sigma R]L$, with $\sigma$constant. To describe matter inside neutron stars we assume the polytropicequation of state $p=K \rho^{\gamma}$, with $K$ and $\gamma = 5/3 $ beingconstants. We show that in this theory it is possible to reach the mass ofmassive pulsars such as PSR J2215+5135. As a feature of the GMC theory, verycompact neutron stars with radius $\sim8$km and $M\sim 2.6M_\odot$ are stable,thus surpassing the Buchdal and Schwarzschild radius limits. Moreover, thereferred stellar diameter is obtained within the range of observational data.

Hydrostatic equilibrium configurations of neutron stars in a non-minimal geometry-matter coupling theory of gravity