Based on the epicyclic approximation, we have
simulated the motion of the young open star clusters IC 4665 and
Collinder 359. The separation between the cluster centers is shown
to have been minimal 7 Myr ago, 36 pc. We have established a close
evolutionary connection between IC 4665 and the Scorpius-Centaurus
association -- the separation between the centers of these
structures was ≈200pc 15 Myr ago. In addition, the center
of IC 4665 at this time was near two well-known regions of coronal
gas: the Local Bubble and the North Polar Spur. The star HIP 86768
is shown to be one of the candidates for a binary (in the past)
with the pulsar PSR B1929+10. At the model radial velocity of the
pulsar Vr = 2±50 km s-1, a close encounter of this pair
occurs in the vicinity of IC 4665 at a time of -1.1 Myr. At the
same time, using currently available data for the pulsar B1929+10
at its model radial velocity Vr = 200±50 km s-1, we show
that the hypothesis of Hoogerwerf et al. (2001) about the breakup
of the ζOph--B1929+10 binary in the vicinity of Upper
Scorpius (US) about 0.9 Myr ago is more plausible.