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It is shown how the Equation of State (EoS) depends on nucleon propertiesinside Nuclear Matter (NM). We propose to benefit from the concept of enthalpyin order to include volume corrections to the nucleon rest energy, which areproportional to pressure and absent in a standard Relativistic Mean Field (RMF)with point-like nucleons. As a result, the nucleon mass can decrease inside NM,making the model nonlinear and the EoS softer. The course of the EoS in our RMFmodel agrees with a semi-empirical estimate and is close to the resultsobtained from extensive DBHF calculations with a Bonn A potential, whichproduce an EoS stiff enough to describe neutron star properties (mass--radiusconstraint), especially the masses of PSR J1614_2230 and PSR J0348_0432, knownas the most massive ($\sim 2 M_\odot$) neutron stars. The presented model hasproper saturation properties, including a good value of compressibility.

Nuclear equation of state and finite nucleon volumes