  In this paper we present a new result, namely that the primal magnetic field
of the collapsed core during a supernova explosion will, as a result of the
conservation of magnetic flux, receive a massive boost to more than 90 times
its original value by the Pauli paramagnetization of the highly degenerate
relativistic electron gas just after the formation of the neutron star. Thus,
the observed super-strong magnetic field of neutron stars may originate from
the induced Pauli paramagnetization of the highly degenerate relativistic
electron gas in the interior of the neutron star. We therefore have an
apparently natural explanation for the surface magnetic field of a neutron
star.
