Jupiter's stormy secret: Ammonia-laden ice balls uncovered
Scientists have discovered that during storms on Jupiter, ice balls containing ammonia and water descend. This unusual phenomenon provides new insights into the uneven distribution of this compound on its surface.
During storms on Jupiter, an extraordinary occurrence takes place. Strong gusts of wind and rain lead to the formation of ice balls combined with ammonia in the planet's atmosphere. These formations have a consistency similar to wet snow and result from complex atmospheric processes. According to Science Alert, scientists from the University of California, Berkeley, led by Chris Moeckel, studied this phenomenon for three years. Although the researchers were initially sceptical of the theory, their studies confirmed the existence of this surprising process.
How do these unusual ice balls form?
The hypothesis regarding the formation of water-ammonia balls emerged in 2020 when researchers analysed data from the Juno probe. During storms, water is hurled high above the water clouds, where it encounters ammonia vapour. In extremely low temperatures, water and ammonia freeze together, forming hail. Heidi Becker from NASA explains that ammonia acts as an antifreeze, lowering the melting point of ice.
Jupiter's storms are surprising
Jupiter's atmosphere is characterised by storms that penetrate deep into the atmosphere. While most weather phenomena are shallow, some, like cyclones or thunderstorms, extend deep into the troposphere. It is within these storms that the ice balls, which transport ammonia deep into the planet, form.
Previously, scientists did not know what removed ammonia from the atmosphere, but this phenomenon explains why ammonia is unevenly distributed in Jupiter's atmosphere. Ice balls with ammonia and water descend, carrying ammonia into the planet's interior and transporting it to the surface during violent storms.
Possibility of occurrence on other planets
The mechanism of ice ball formation may not be unique to Jupiter. Scientists suggest that similar processes might occur on other gas giants within the Solar System and beyond. Future observations may confirm these assumptions.
