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.