原行星盘中H3 +对稀有气体的隔离和外太阳系的组成
Sequestration of noble gases by H3+ in protoplanetary disks and outer solar system composition
摘要：
我们研究的惰性气体封存的效率由离子H3+的形式XH 3+络合物（与X =氩，氪或氙）在气相条件下遇到类似的冷却过程中的原行星盘，在冰冷的星子形成的时代。我们发现，XH 3+配合物在气相中形成非常稳定的结构，它们的结合能远高于那些参与的X-H 2 O水合物或纯X-X冷凝物的结构。这意味着，在H3+离子的存在下，氩、氪或氙可能以XH 3+络合物的形式嵌入气相中，而不是在原行星盘冷却期间形成冰。不足的量取决于有多少H3+是可用的，并且在捕获惰性气体方面是有效的。在太阳星云中面的致密气体中，H3+是由高能粒子（如宇宙射线或年轻太阳喷射出的粒子）电离H2而形成的。即使使用宇宙射线电离率的最大估计值，我们计算出H3+丰度分别比氙和氪丰度低两个和三个数量级。另一方面，估计年轻太阳引起的电离是非常不确定的，但留下了足够的H3+使氪和氙捕获有效的可能性。最后，H3+形成的额外来源可能是附近超新星的存在，如文献中所讨论的。最近对太阳系的观测表明，泰坦和彗星中的Ar缺乏，而Kr和Kr则更缺乏。在这篇文章中，我们认为，这种不足是由上述过程，即捕获这些稀有气体的太阳星云中的H3+离子造成的可能性。
英文摘要：
We study the efficiency of the noble gases sequestration by the ion H3+ in the form of XH3+ complexes (with X = argon, krypton or xenon) in gas phase conditions similar to those encountered during the cooling of protoplanetary disks, at the epoch of icy planetesimals formation. We show that XH3+ complexes form very stable structures in the gas phase and that their binding energies are much higher than those involved in the structures of X-H2O hydrates or pure X-X condensates. This implies that, in presence of H3+ ions, argon, krypton or xenon are likely to remain sequestrated in the form of XH3+ complexes embedded in the gas phase rather than forming ices during the cooling of protoplanetary disks. The amount of the deficiency depends on how much H3+ is available and efficient in capturing noble gases. In the dense gas of the mid-plane of solar nebula, H3+ is formed by the ionization of H2 from energetic particles, as those in cosmic rays or those ejected by the young Sun. Even using the largest estimate of the cosmic rays ionization rate, we compute that the H3+ abundance is two and three orders of magnitude lower than the xenon and krypton abundance, respectively. Estimating the ionization induced by the young Sun, on the other hand, is very uncertain but leaves the possibility to have enough H3+ to make krypton and xenon trapping efficent. Finally, additional source of H3+ formation may be provided by the presence of a nearby supernova, as discussed in the literature. Recent solar system observations show a deficiency of Ar, and, even more, of Kr and Xe in Titan and in comets. In this article, we consider the possibility that this deficiency is caused by the afore-mentioned process, namely trapping of those noble gases by H3+ ions in the solar nebula.
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