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Based on the epicyclic approximation, we have simulated the motion of theyoung open star clusters IC 4665 and Collinder 359. The separation between thecluster centers is shown to have been minimal 7 Myr ago, 36 pc. We haveestablished a close evolutionary connection between IC 4665 and theScorpius-Centaurus association -- the separation between the centers of thesestructures was $\approx200$ pc 15 Myr ago. In addition, the center of IC 4665at this time was near two well-known regions of coronal gas: the Local Bubbleand the North Polar Spur. The star HIP 86768 is shown to be one of thecandidates for a binary (in the past) with the pulsar PSR B1929+10. At themodel radial velocity of the pulsar $V_r= 2\pm50$ km s$^{-1}$, a closeencounter 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 itsmodel radial velocity $V_r=200\pm50$ km s$^{-1}$, we show that the hypothesisof Hoogerwerf et al. (2001) about the breakup of the $\zeta$Oph--B1929+10binary in the vicinity of Upper Scorpius (US) about 0.9 Myr ago is moreplausible.

Open Clusters IC 4665 and Cr 359 and a Probable Birthplace of the Pulsar PSR B1929+10