  Modified dispersion relations from effective field theory are shown to alter
the Chandrasekhar mass limit. At exceptionally high densities, the
modifications affect the pressure of a degenerate electron gas and can increase
or decrease the mass limit, depending on the sign of the modifications. These
changes to the mass limit are unlikely to be relevant for the astrophysics of
white dwarf or neutron stars due to well-known dynamical instabilities that
occur at lower densities. Generalizations to frameworks other than effective
field theory are discussed.
