  We discuss effects of magnetic fields on proto-neutron star winds by
performing numerical simulation. We assume that the atmosphere of proto-neutron
star has a homogenous magnetic field (ranging from ~10^{12} G to ~10^{15} G)
perpendicular to the radial direction and examine the dependence of the three
key quantities (dynamical time scale, electron fraction, and entropy per
baryon) for the successful r-process on the magnetic field strength. Our
results show that even with a magneter-class field strength, ~10^{15} G, the
feature of the wind dynamics varies only little from that of non-magnetic
winds, and that the condition for successful r-process is not realized.
