论文标题
129i和247厘米的陨石限制了太阳能过程的最后一个天体物理来源
129I and 247Cm in Meteorites Constrain the Last Astrophysical Source of Solar r-process Elements
论文作者
论文摘要
早期太阳系的组成可以从陨石推断出来。许多比铁重的元素是由快速中子捕获过程（R过程）形成的，但是发生这种情况的天体物理来源仍然很少了解。我们证明了放射性的R-Process Nuclei 129i和247cm的近乎相同的半衰期（$ \ simeq $ 15.6 Myr）保持其比例，而与太阳系中的生产和掺入之间无关。我们通过比较测得的陨石129i / 247cm = 438 $ \ pm $ 184与基于中子星星合并和磁旋转超新星模拟的核合成计算来限制最后的R过程。通常在合并磁盘弹出模拟中发现的中子富含中子条件与陨石值最一致。不确定的核物理数据限制了我们对这一结论的信心。
The composition of the early Solar System can be inferred from meteorites. Many elements heavier than iron were formed by the rapid neutron-capture process (r process), but the astrophysical sources where this occurred remain poorly understood. We demonstrate that the near-identical half-lives ($\simeq$ 15.6 Myr) of the radioactive r-process nuclei 129I and 247Cm preserve their ratio, irrespective of the time between production and incorporation into the Solar System. We constrain the last r-process source by comparing the measured meteoritic 129I / 247Cm = 438 $\pm$ 184 to nucleosynthesis calculations based on neutron star merger and magneto-rotational supernova simulations. Moderately neutron-rich conditions, often found in merger disk ejecta simulations, are most consistent with the meteoritic value. Uncertain nuclear physics data limit our confidence in this conclusion.
