“…In this work we use the fact that many models of gravitation, in particular f (R) Palatini gravity (see the section II for a short review of the model), slightly alter the non-relativistic limit of (sub-)stellar structural equations by introducing new (geometric) terms proportional to functions of energy density [23][24][25] (for a review see [26,27]). Modified non-relativistic equations in the context of stars and brown dwarfs have been already widely used by the physics community, mainly to obtain limiting masses, such as e.g., the Chandrasekhar mass for white dwarf stars [28][29][30][31][32][33], the minimum Main Sequence mass 1 [34][35][36][37], or minimum mass for deuterium burning [38].…”