Theoretical evidence of H-He demixing under Jupiter and Saturn conditions

Xiaoju Chang, Bo Chen, Qiyu Zeng, Han Wang, Kaiguo Chen, Qunchao Tong, Xiaoxiang Yu, Dongdong Kang, Shen Zhang, Fangyu Guo, Yong Hou, Zengxiu Zhao, Yansun Yao (), Yanming Ma () and Jiayu Dai ()
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Xiaoju Chang: National University of Defense Technology
Bo Chen: National University of Defense Technology
Qiyu Zeng: National University of Defense Technology
Han Wang: Institute of Applied Physics and Computational Mathematics
Kaiguo Chen: National University of Defense Technology
Qunchao Tong: National University of Defense Technology
Xiaoxiang Yu: National University of Defense Technology
Dongdong Kang: National University of Defense Technology
Shen Zhang: National University of Defense Technology
Fangyu Guo: National University of Defense Technology
Yong Hou: National University of Defense Technology
Zengxiu Zhao: National University of Defense Technology
Yansun Yao: University of Saskatchewan
Yanming Ma: Jilin University
Jiayu Dai: National University of Defense Technology

Nature Communications, 2024, vol. 15, issue 1, 1-9

Abstract: Abstract The immiscibility of hydrogen-helium mixture under the temperature and pressure conditions of planetary interiors is crucial for understanding the structures of gas giant planets (e.g., Jupiter and Saturn). While the experimental probe at such extreme conditions is challenging, theoretical simulation is heavily relied in an effort to unravel the mixing behavior of hydrogen and helium. Here we develop a method via a machine learning accelerated molecular dynamics simulation to quantify the physical separation of hydrogen and helium under the conditions of planetary interiors. The immiscibility line achieved with the developed method yields substantially higher demixing temperatures at pressure above 1.5 Mbar than earlier theoretical data, but matches better to the experimental estimate. Our results suggest a possibility that H-He demixing takes place in a large fraction of the interior radii of Jupiter and Saturn, i.e., 27.5% in Jupiter and 48.3% in Saturn. This indication of an H-He immiscible layer hints at the formation of helium rain and offers a potential explanation for the decrease of helium in the atmospheres of Jupiter and Saturn.

Date: 2024
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DOI: 10.1038/s41467-024-52868-4

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