Implications of q-deformed statistics on stellar stability

Abstract

Examination of Chandrasekhar's equilibrium and stability condition for stars in the context of q-deformed Maxwell-Boltzmann statistics leads to the derivation of a new analytical formula that extends its classical case. This derivation assumes that the kinetic description of stellar matter conforms to a generalized Maxwell-Boltzmann distribution. It has been found that the maximum allowable radiation pressure at the center of a star for a given mass depends on the deformation parameter q . The classical Chandrasekhar condition is recovered in this framework when q equals 1.