Recent high-resolution findings from ESA’s Solar Orbiter mission provide groundbreaking insights into solar flares. These explosive events are triggered by cascading magnetic reconnection processes, releasing immense energy and “raining down” plasma clumps into the Sun’s atmosphere.
Detailed overview of M-class solar flares as observed by ESA’s solar probes. Image credit: ESA / Solar Orbiter / Chitta et al., doi: 10.1051/0004-6361/202557253.
Solar flares are powerful explosions originating from the Sun.
These dramatic events occur when energy stored in entangled magnetic fields is suddenly unleashed through a process known as “magnetic reconnection.”
In mere minutes, intersecting magnetic field lines disconnect and reconnect, leading to a rapid rise in temperature and accelerating millions of degrees of plasma and high-energy particles, potentially resulting in solar flares.
The most intense flares can initiate a cascade of reactions, causing magnetic storms on Earth and potentially disrupting radio communications. Hence, monitoring and understanding these flares is crucial.
However, the mechanisms behind such swift energy release remain largely enigmatic.
An exceptional series of observations from the Solar Orbiter’s four instruments has finally provided clarity. This mission, with its comprehensive approach, offers the most detailed perspective on solar flares to date.
The Solar Orbiter’s Extreme Ultraviolet Imager (EUI) captured high-resolution images of features just hundreds of kilometers across in the Sun’s outer atmosphere (corona), recording changes every two seconds.
Three other instruments—SPICE, STIX, and PHI—examined various depth and temperature regions, from the corona to the Sun’s visible surface, or photosphere.
“We were fortunate to witness this massive flare precursor in such exquisite detail,” said Dr. Pradeep Chitta, an astronomer at the Max Planck Institute for Solar System Research.
“Such detailed and frequent observations of flares are rarely possible due to the limited observation window and the significant data storage required.”
“We were in the right place at the right time to capture these intricate details of the flare.”
Solar Orbiter observations have revealed an intricate view of the central engine during the preflare and shock stages of a solar flare as a magnetic avalanche.
“Even prior to the major flare event, ribbon-like features rapidly traversed the Sun’s atmosphere,” Dr. Chitta noted.
“The flow of these ‘rainy plasma blobs’ indicates increasing energy buildup, intensifying as the flare progresses.”
“This rain of plasma will continue for a while even after the flare diminishes.”
“This marks the first time we’ve observed such a level of spatial and temporal detail in the solar corona.”
“We did not anticipate such high-energy particles emerging from the avalanche process.”
“There is still much to explore regarding this phenomenon, but future missions equipped with high-resolution X-ray imaging will further our understanding.”
“This is one of Solar Orbiter’s most thrilling achievements thus far,” stated Dr. Miho Jamby, ESA’s Solar Orbiter Collaborative Project Scientist.
“The Solar Orbiter’s observations unveil the flare’s central engine and underscore the significant role of an avalanche-like magnetic energy release mechanism.”
There is a compelling prospect of whether this mechanism is universal across all flares and in other flaring stars.
Results can be found in the journal Astronomy and Astrophysics.
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LP Citta et al. 2026. Magnetic avalanches as the central engine driving solar flares. A&A 705, A113; doi: 10.1051/0004-6361/202557253
Source: www.sci.news
