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

Author

Listed:
  • Xiaoju Chang

    (National University of Defense Technology
    National University of Defense Technology)

  • Bo Chen

    (National University of Defense Technology
    National University of Defense Technology)

  • Qiyu Zeng

    (National University of Defense Technology
    National University of Defense Technology)

  • Han Wang

    (Institute of Applied Physics and Computational Mathematics)

  • Kaiguo Chen

    (National University of Defense Technology
    National University of Defense Technology)

  • Qunchao Tong

    (National University of Defense Technology
    National University of Defense Technology)

  • Xiaoxiang Yu

    (National University of Defense Technology
    National University of Defense Technology)

  • Dongdong Kang

    (National University of Defense Technology
    National University of Defense Technology)

  • Shen Zhang

    (National University of Defense Technology
    National University of Defense Technology)

  • Fangyu Guo

    (National University of Defense Technology
    National University of Defense Technology)

  • Yong Hou

    (National University of Defense Technology
    National University of Defense Technology)

  • Zengxiu Zhao

    (National University of Defense Technology
    National University of Defense Technology)

  • Yansun Yao

    (University of Saskatchewan)

  • Yanming Ma

    (Jilin University
    Jilin University)

  • Jiayu Dai

    (National University of Defense Technology
    National University of Defense Technology)

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.

Suggested Citation

  • 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 & Jiayu Dai, 2024. "Theoretical evidence of H-He demixing under Jupiter and Saturn conditions," Nature Communications, Nature, vol. 15(1), pages 1-9, December.
  • Handle: RePEc:nat:natcom:v:15:y:2024:i:1:d:10.1038_s41467-024-52868-4
    DOI: 10.1038/s41467-024-52868-4
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    References listed on IDEAS

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    1. S. Brygoo & P. Loubeyre & M. Millot & J. R. Rygg & P. M. Celliers & J. H. Eggert & R. Jeanloz & G. W. Collins, 2021. "Evidence of hydrogen−helium immiscibility at Jupiter-interior conditions," Nature, Nature, vol. 593(7860), pages 517-521, May.
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