  If the theoretical relationship between white dwarf mass and orbital period
for wide-orbit binary radio pulsars is assumed to be correct, then the neutron
star mass of PSR J2019+2425 is shown to be ~1.20 M_sun. Hence the mass of the
neutron star in this system prior to the mass transfer phase is expected to
have been < 1.1 M_sun. Alternatively this system descends from the accretion
induced collapse (AIC) of a massive white dwarf. We estimate the magnetic
inclination angles of all the observed wide-orbit low-mass binary pulsars in
the Galactic disk using the core-mass period relation and assuming that the
spin axis of an accreting neutron star aligns with the orbital angular momentum
vector in the recycling process of the pulsar. The large estimated magnetic
inclination angle of PSR J2019+2425, in combination with its old age, gives for
this system evidence against alignment of the magnetic field axis with the
rotational spin axis. However, in the majority of the similar systems the
distribution of magnetic inclination angles is concentrated toward low values
(if the core-mass period relation is correct) and suggests that alignment has
taken place.
