GP is correct-- the neutron degeneracy pressure prevents the stellar remnant from getting any smaller, but it is the electron degeneracy pressure which makes beta decay energetically unfavorable.  In order to be produced by neutron beta decay, an electron must enter a valid state.  Pauli exclusion (electrons are fermions) requires the electron to enter a state at least as energetic as the electron Fermi level, which due to the neutron star&#x27;s gravity is comparable to the rest mass of the electron.  Neutron decay is energetically favorable, but not that favorable.  The reverse process accelerates and equilibrium is reached.