  We investigate the possibility of the r-process during the
magnetohydrohynamical explosion of supernova in a massive star of 13 solar mass
with the effects of neutrinos induced. We adopt five kinds of initial models
which include properties of rotation and the toroidal component of the magnetic
field . The simulations which succeed the explosions are limitted to a
concentrated magnetic field and strong differential rotation. Low $Y_{e}$
ejecta produce heavy elements and the third peak can be reprocuced. However,
the second peak is low because $Y_{e}$ distribution as a function of radius is
steep and ejecta corresponding to middle $Y_{e}$ is very few.
