arXivDaily arXiv每日学术速递 周一至周五更新
arXiv 2011.13285cond-mat.mtrl-sciastro-ph.EP
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高压下稳定的H-C-N-O化合物

On stable H-C-N-O compounds at high pressure

Lewis J. Conway, Chris J. Pickard, Andreas Hermann

摘要:

外行星和它们的许多卫星的组成主要是由H-C-N-O化学空间的物质组成的,通常被认为是由氢和行星冰H $_2$ O、CH $_4$和NH $_3$的混合物组成的。在它们的内部,这些冰经历了极端的压力条件,在海王星幔核边界处约为5 Mbar,预计它们会经历相变,分解并形成全新的化合物。反过来,这决定了行星的内部结构,热历史,磁场产生等,尽管它的重要性,H-C-N-O空间还没有被系统地调查。简单地问:在高压条件下,什么化合物会出现在这个空间中,是什么决定了它们的稳定性?在这里,我们报告的结果,从一个公正的晶体结构搜索之间的H-C-N-O化合物在5毫巴回答这个问题。

英文摘要:

The make-up of the outer planets, and many of their moons, are dominated by matter from the H-C-N-O chemical space, commonly assumed to originate from mixtures of hydrogen and the planetary ices H$_2$O, CH$_4$, and NH$_3$. In their interiors, these ices experience extreme pressure conditions, around 5 Mbar at the Neptune mantle-core boundary, and it is expected that they undergo phase transitions, decompose, and form entirely new compounds. In turn, this determines planets' interior structure, thermal history, magnetic field generation, etc. Despite its importance, the H-C-N-O space has not been surveyed systematically. Asked simply: at high-pressure conditions, what compounds emerge within this space, and what governs their stability? Here, we report on results from an unbiased crystal structure search amongst H-C-N-O compounds at 5 Mbar to answer this question.

机构、总结、中文摘要均由AI分析而来,可能存在错误,请以论文正文为准。

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