cosmic ray焊剂中59 Co和59 Ni的丰度
Abundances of 59Co and 59Ni in the cosmic ray flux
摘要：
关于银河系宇宙射线起源的两个主要假说是“超新星”和“超级气泡”起源假说。我们分析了宇宙射线通量中钴和镍同位素相对丰度的测量所提供的超级气泡假说的证据。我们比较了宇宙线流量中59 Ni丰度的测量上限与最新恒星演化模型的59 Ni丰度预测。在宇宙射线通量中未探测到59 Ni以前被归因于超新星爆炸和粒子加速过程开始之间的1 e5年量级的大时间延迟。这一巨大的时间延迟被认为是支持“超级泡沫”假设的一个论据。我们表明，最近计算的大质量恒星的59 Ni产量，其中考虑到初始质量范围高达120太阳质量，包括恒星自转，结果预测低59 Ni丰度相对于其衰变产物59 Co。预测的丰度是一致的上限59镍丰度的宇宙射线通量的超新星参数假设。这一结果排除了在超新星爆发和加速过程开始之间的时间间隔中59 Ni衰变的必要性，并恢复了59 Ni/59 Co丰度测量与CR起源的“超新星”假设的一致性。
英文摘要：
Two main hypotheses for the origin of Galactic cosmic rays are the "supernova" and "superbubble" origin hypotheses. We analyse the evidence for the superbubble hypothesis provided by the measurements of the relativive abundances of isotopes of cobalt and nickel in the cosmic ray flux. We compare the measured upper limit on the abundance of 59Ni in the cosmic ray flux with the 59Ni abundance predictions of the up-to-date stellar evolution models. Non-detection of 59Ni in the cosmic ray flux has previously been attributed to a large time delay of the order of 1e5 yr between the moment of supernova explosion and the onset of particle acceleration process. This large time delay was considered as an argument in favour of the "superbubble" scenario. We show that the recent calculation of the 59Ni yield of massive stars, which takes into account the initial mass range up to 120 solar masses and includes stellar rotation, results in prediction of low 59Ni abundance relative to its decay product 59Co. The predicted abundance is consistent with the upper bound on 59Ni abundance in the cosmic ray flux for the supernova parameters assumed. This result removes the necessity of decay of 59Ni in the time interval between the supernova explosion and the onset of acceleration process and restores the consistency of measurements of 59Ni / 59Co abundances with the "supernova" hypothesis of the CR origin.
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