Theoretical evidence of H-He demixing under Jupiter and Saturn conditions
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arXiv
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| Main Authors: | , , , , , , , , , , , , , , |
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| Format: | Preprint |
| Published: |
2023
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| _version_ | 1866910826328227840 |
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| author | Chang, Xiaoju Chen, Bo Zeng, Qiyu Wang, Han Chen, Kaiguo Tong, Qunchao Yu, Xiaoxiang Kang, Dongdong Zhang, Shen Guo, Fangyu Hou, Yong Zhao, Zengxiu Yao, Yansun Ma, Yanming Dai, Jiayu |
| author_facet | Chang, Xiaoju Chen, Bo Zeng, Qiyu Wang, Han Chen, Kaiguo Tong, Qunchao Yu, Xiaoxiang Kang, Dongdong Zhang, Shen Guo, Fangyu Hou, Yong Zhao, Zengxiu Yao, Yansun Ma, Yanming Dai, Jiayu |
| contents | 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. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2310_13412 |
| institution | arXiv |
| publishDate | 2023 |
| record_format | arxiv |
| spellingShingle | Theoretical evidence of H-He demixing under Jupiter and Saturn conditions Chang, Xiaoju Chen, Bo Zeng, Qiyu Wang, Han Chen, Kaiguo Tong, Qunchao Yu, Xiaoxiang Kang, Dongdong Zhang, Shen Guo, Fangyu Hou, Yong Zhao, Zengxiu Yao, Yansun Ma, Yanming Dai, Jiayu Computational Physics Earth and Planetary Astrophysics Atomic and Molecular Clusters 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. |
| title | Theoretical evidence of H-He demixing under Jupiter and Saturn conditions |
| topic | Computational Physics Earth and Planetary Astrophysics Atomic and Molecular Clusters |
| url | https://arxiv.org/abs/2310.13412 |