Heat and charge transport in H2O at ice-giant conditions from ab initio molecular dynamics simulations
Heat and charge transport in H2O at ice-giant conditions from ab initio molecular dynamics simulations
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DOI：
10.1038/s41467-020-17275-5
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发表时间：
2020-07-17
影响因子：
16.6
通讯作者：
Baroni, Stefano
中科院分区：
文献类型：
--
作者：
Grasselli, Federico;Stixrude, Lars;Baroni, Stefano
行星的内部结构和热历史对其可观测特征（例如光度或磁场）的影响很大程度上取决于其内层鲜为人知的热和电荷传输特性。天王星或海王星等冰巨行星内部发生的不同相水（液体、固体和超离子）的热导率和电导率是从平衡从头开始分子动力学进行评估的，利用了扩展系统中输运理论和数据分析的最新进展。简要讨论了我们的发现对冰巨星演化模型的影响。
The impact of the inner structure and thermal history of planets on their observable features, such as luminosity or magnetic field, crucially depends on the poorly known heat and charge transport properties of their internal layers. The thermal and electric conductivities of different phases of water (liquid, solid, and super-ionic) occurring in the interior of ice giant planets, such as Uranus or Neptune, are evaluated from equilibrium ab initio molecular dynamics, leveraging recent progresses in the theory and data analysis of transport in extended systems. The implications of our findings on the evolution models of the ice giants are briefly discussed.