  The origin of high velocities of pulsars is studied by considering the
spin-flip conversion of neutrinos propagating in a gravitational field of a
protoneutron star. For a rotating gravitational source (such as pulsars) with
angular velocity ${\bm \omega}$, one finds that the spin connections (entering
in the Dirac equation written in curved space time) induce an additional
contribution to neutrino energy which is proportional to ${\bm \omega}\cdot
{\bf p}$, with ${\bf p}$ the neutrino momentum. Such a coupling (spin-gravity
coupling) can be responsible of pulsar kicks being the asymmetry of the
neutrino emission generated by the relative orientation of the neutrino
momentum ${\bf p}$ with respect to the angular velocity ${\bm \omega}$. As a
consequence, the mechanism suggests that the motion of pulsars is correlated to
their angular velocity ${\bm \omega}$. In this work we consider neutrinos
propagating orthogonally to the magnetic field. As in the usual approaches,spin
flip conversion is generated via the coupling of the neutrino magnetic momentum
with the magnetic field. For our estimations, we use the large non-standard
neutrino magnetic momentum provided by astrophysical and cosmological
constraints, $\mu_\nu\sim 10^{-11}\mu_B$. The connection with recent
observations and statistical analysis is also discussed.
