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Melting curve of superionic ammonia at planetary interior conditions
Laser-driven shock compression experiments yield the melting curve of the superionic phase of ammonia at conditions relevant to the interiors of Uranus and Neptune.
- J.-A. Hernandez
- , M. Bethkenhagen
- & A. Ravasio
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News & Views |
From storms to cyclones at Jupiter’s poles
The atmospheres of most planets in our Solar System have a single large cyclonic vortex at each of their poles. Jupiter with its polygonal cyclones surrounding a single one, however, falls out of line, owing to an energy transfer to larger scales.
- Agustín Sánchez-Lavega
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Article
| Open AccessMoist convection drives an upscale energy transfer at Jovian high latitudes
Infrared images of Jupiter taken by the Juno spacecraft reveal an energy transfer driven by moist convection. This mechanism is expected to enhance heat transfer, which might also be relevant to Earth’s atmosphere.
- Lia Siegelman
- , Patrice Klein
- & Giuseppe Sindoni
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News & Views |
Hot black ices
At high pressure and temperature, water forms two crystalline phases, known as hot ‘black’ ices due to their partial opaqueness. A detailed characterization of these phases may explain magnetic field formation in giant icy planets like Neptune.
- Simone Anzellini
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Article |
Structure and properties of two superionic ice phases
Measurements of the phase diagram of water reveal first-order phase transitions to face- and body-centred cubic superionic ice phases. The former is suggested to be present in the interior of ice giant planets.
- Vitali B. Prakapenka
- , Nicholas Holtgrewe
- & Alexander F. Goncharov
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Phase behaviours of superionic water at planetary conditions
Superionic water is believed to exist in the interior of ice giant planets. By combining machine learning and free-energy methods, the phase behaviours of water at the extreme pressures and temperatures prevalent in such planets are predicted.
- Bingqing Cheng
- , Mandy Bethkenhagen
- & Sebastien Hamel
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Article |
Forward and inverse kinetic energy cascades in Jupiter’s turbulent weather layer
The Jovian atmosphere is highly turbulent due to processes happening on a wide range of length scales. Cassini spacecraft data now suggest the presence of kinetic energy cascades over different length scales — a likely origin of Jupiter’s turbulence.
- Roland M. B. Young
- & Peter L. Read
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Letter |
Cassini in situ observations of long-duration magnetic reconnection in Saturn’s magnetotail
Cassini’s encounter with Saturn’s magnetotail — the long magnetosphere region stretching into space — has revealed that plasma exits the magnetosphere through long-duration magnetic reconnection, which ejects ten times more mass than estimated.
- C. S. Arridge
- , J. P. Eastwood
- & M. K. Dougherty