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The immiscibility of hydrogen-helium mixture under the temperature andpressure conditions of planetary interiors is crucial for understanding thestructures of gas giant planets (e.g., Jupiter and Saturn). While theexperimental probe at such extreme conditions is challenging, theoreticalsimulation is heavily relied in an effort to unravel the mixing behavior ofhydrogen and helium. Here we develop a method via a machine learningaccelerated molecular dynamics simulation to quantify the physical separationof hydrogen and helium under the conditions of planetary interiors. Theimmiscibility line achieved with the developed method yields substantiallyhigher demixing temperatures at pressure above 1.5 Mbar than earliertheoretical data, but matches better to the experimental estimate. Our resultsrevise the structures of Jupiter and Saturn where H-He demixing takes place ina large fraction of the interior radii, i.e., 27.5% in Jupiter and 48.3% inSaturn. This direct evidence of an H-He immiscible layer supports the formationof helium rain and explains the helium reduction in atmosphere of Jupiter andSaturn.

Direct evidence of helium rain in Jupiter and Saturn