疏散星团IC 4665和Cr 359以及脉冲星PSR B1929 +10的可能位置
Open Clusters IC 4665 and Cr 359 and a Probable Birthplace of the Pulsar PSR B1929+10
摘要：
在周转近似下，我们模拟了年轻疏散星团IC 4665和Collinder 359的运动。星团中心之间的距离在700万年前是最小的，36 pc。我们已经在IC 4665和天蝎座-半人马座组合之间建立了密切的进化联系--这些结构的中心之间的分离是1500万年前的$\approx200$ pc。此外，IC 4665的中心在这个时候靠近两个著名的日冕气体区域：本地气泡和北极支线。HIP 86768是与脉冲星PSR B1929+10组成双星的候选者之一。在脉冲星$V_r= 2\pm50$ km s $^{-1}$的模型径向速度下，这一对的近距离相遇发生在IC 4665附近，时间为-110万年。同时，利用目前可用的脉冲星B1929+10在其模型径向速度$V_r=200\pm50$ km s $^{-1}$的数据，我们表明，Hoogerwerf等人（2001）关于$ζ$ Oph-B1929 +10双星在大约90万年前在上天蝎座（US）附近破裂的假设是更合理的。
英文摘要：
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 $\approx200$ 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 $V_r= 2\pm50$ 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 $V_r=200\pm50$ km s$^{-1}$, we show that the hypothesis of Hoogerwerf et al. (2001) about the breakup of the $ζ$Oph--B1929+10 binary in the vicinity of Upper Scorpius (US) about 0.9 Myr ago is more plausible.
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