  Understanding chondrule formation provides invaluable clues about the origin
of the solar system. Recent studies suggest that planetesimal collisions and
the resulting impact melts are promising for forming chondrules. Given that the
dynamics of planetesimals is a key in impact-based chondrule formation
scenarios, we here perform direct $N$-body simulations to examine how the
presence of Jupiter affects the properties of chondrule-forming collisions. Our
results show that the absence/presence of Jupiter considerably changes the
properties of high velocity collisions whose impact velocities are higher than
2.5 km s$^{-1}$; high velocity collisions occur due to impacts between
protoplanets and planetesimals for the case without Jupiter; for the case with
Jupiter, eccentricities of planetesimals are pumped up by the secular and
resonant perturbations from Jupiter. We also categorize the resulting
planetesimal collisions and find that most of high velocity collisions are
classified as grazing ones for both cases. To examine the effect of Jupiter on
chondrule formation directly, we adopt the impact jetting scenario and compute
the resulting abundance of chondrules. Our results show that for the case
without Jupiter, chondrule formation proceeds in the inside-out manner,
following the growth of protoplanets. If Jupiter is present, the location and
timing of chondrule formation are determined by Jupiter's eccentricity, which
is treated as a free parameter in our simulations. Thus, the existence of
Jupiter is the key parameter for specifying when and where chondrule formation
occurs for impact-based scenarios.
