  We study the effects of jet-like explosion in SN 1987A. Calculations of the
explosive nucleosynthesis and the matter mixing in a jet-like explosion are
performed and their results are compared with the observations of SN 1987A. It
is shown that the jet-like explosion model is favored because the radioactive
nuclei 44Ti is produced in a sufficient amount to explain the observed
bolometric luminosity at 3600 days after the explosion. It is also shown that
the observed line profiles of Fe[II] are well reproduced by the jet-like
explosion model. In particular, the fast moving component travelling at
(3000-4000) km/s is well reproduced, which has not been reproduced by the
spherical explosion models. Moreover, we conclude that the favored degree of a
jet-like explosion to explain the tail of the light curve is consistent with
the one favored in the calculation of the matter mixing. The concluded ratio of
the velocity along to the polar axis relative to that in the equatorial plane
at the Si/Fe interface is about 2:1. This conclusion will give good constraints
on the calculations of the dynamics of the collapse-driven supernova. The
asymmetry of the observed line profiles of Fe[II] can be explained when the
assumption of the equatorial symmetry of the system is removed, which can be
caused by the asymmetry of the jet-like explosion with respect to the
equatorial plane. In the case of SN 1987A, the jet on the north pole has to be
stronger than that on the south pole in order to reproduce the observed
asymmetric line profiles. Such an asymmetry may also be the origin of the
pulsar kick. When we believe some theories that cause such an asymmetric
explosion, the proto -neutron star born in SN 1987A is moving in the southern
part of the remnant.
