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We study the stability of non-relativistic polytropic stars within twomodified gravity theories i.e., Beyond Horndeski gravity and Eddington inspiredBorn Infeld theories using the configuration entropy method. We use spatiallylocalized bounded function of energy density as solutions from stellareffective equations to construct the corresponding configuration entropy. Weuse the same argument as the one used by the authors of Refs. [1,2] that thestars are stable if there is peak in configuration entropy as a function ofadiabatic index curve. Specifically, the boundary between stable and unstableregions which corresponds to Chandrasekhar stability bound is indicated fromthe existence of the maximum peak while the most stable polytropic stars isindicated by minimum peak in the corresponding curve. We have found that thevalue of critical adiabatic indexes of Chandrasekhar stability bound and themost stable polytropic stars predicted by non-relativistic limit of BeyondHorndeski Gravity and Eddington inspired Born Infeld theories are different tothose predicted by general relativity where the corresponding differencesdepend on the free parameter of both theories.

Information-Entropic Method: Stability of Stars and Modified Gravity Theories