  We study the stability of non-relativistic polytropic stars within two
modified gravity theories i.e., Beyond Horndeski gravity and Eddington inspired
Born Infeld theories using the configuration entropy method. We use spatially
localized bounded function of energy density as solutions from stellar
effective equations to construct the corresponding configuration entropy. We
use the same argument as the one used by the authors of Refs. [1,2] that the
stars are stable if there is peak in configuration entropy as a function of
adiabatic index curve. Specifically, the boundary between stable and unstable
regions which corresponds to Chandrasekhar stability bound is indicated from
the existence of the maximum peak while the most stable polytropic stars is
indicated by minimum peak in the corresponding curve. We have found that the
value of critical adiabatic indexes of Chandrasekhar stability bound and the
most stable polytropic stars predicted by non-relativistic limit of Beyond
Horndeski Gravity and Eddington inspired Born Infeld theories are different to
those predicted by general relativity where the corresponding differences
depend on the free parameter of both theories.
