Clusters IC 4665 and Cr 359 and a Probable Birthplace of the Pulsar PSR B 1929 + 10

–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 ≈ 200 pc 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 V r = 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 V r = 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.