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ESA’s Solar Orbiter may have taken another step towards solving the eighty-year-old mystery of why the Sun’s outer atmosphere is so hot.
On 3 March 2022, just a few months into Solar Orbiter’s nominal mission, the spacecraft’s Extreme Ultraviolet Imager (EUI) returned data showing for the first time that a magnetic phenomenon called reconnection was taking place persistently on tiny scales.
At that time, the spacecraft was about halfway between the Earth and the Sun. This enabled coordinated observations with NASA’s Solar Dynamics Observatory (SDO) and Interface Region Imaging Spectrograph (IRIS) missions. The data from the three missions was then combined during the analysis.
Magnetic reconnection occurs when a magnetic field changes itself into a more stable configuration. It is a fundamental energy release mechanism in superheated gasses known as plasmas and is believed to be the major mechanism for powering large-scale solar eruptions. This makes it the direct cause of space weather, and a prime candidate for the mysterious heating of the Sun’s outer atmosphere.
It has been known since the 1940s that the Sun’s outer atmosphere, called the corona, is much hotter than the Sun’s surface. While the surface glows at around 5 500°C, the corona is a rarified gas of around 2 million °C. How the Sun injects energy into its atmosphere to heat it to this tremendous temperature has been a major puzzle ever since.