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CHromospheric magnetic fields in fLAREs and their evolution

Project description

New computer models could shed light on solar explosions in the chromosphere

The Sun is well known for its magnetic activity, including periodic flares that rise from its surface when magnetic field lines tangle, cross or reorganise near sunspots. Flares send streams of charged particles into space. If they are directed towards Earth, these particles can disrupt satellites or cause colourful auroral displays. The EU-funded CHLARE project aims to enhance understanding of solar flares and related solar events in the chromosphere, where studies are scarce. The project will upgrade the existing inversion code to interpret flare physics in the spectral region of He I 1083.0 nm triplet and make it freely available. The work will be complemented by hydrodynamic simulations, and the project's results will provide a valuable foundation for analysing solar flares and space weather.


This research project aims to study the variations of the solar magnetic field in flares, the most energetic events in our solar system. Flares accelerate charged particles into space, which may adversely affect satellites and Earth’s technology. Despite their clear importance for today’s technology, the timing and positioning when flares occur are so far unpredictable. Changes in the solar magnetic field topology are known to be the causes for flares, but their physics is not understood in detail. Past studies have shown prominent changes of the magnetic field in the photosphere during flares. But higher in the atmosphere, in the chromosphere, studies are scarce because ground-based telescopes with special instrumentation and capabilities are needed. No space mission has been or is being planned with capabilities for those chromospheric magnetic measurements. The most suitable spectral range to study the upper chromosphere is the He I 1083.0 nm triplet and the project has access to two unique data sets of high-energetic flares in this spectral region. Since there are no diagnostic tools for this prominent spectral triplet in flares, the first goal is to upgrade an existing tool (spectral-line inversion code) to include flare physics. The code will be made freely available for the benefit of the scientific community, so that it can be used to analyze future flare observations in this wavelength range. The second aim is to use the upgraded tool to infer for the first time the evolution of the magnetic field vector in the two abovementioned data sets. The results will provide thresholds for the shear/ twist of the field lines that lead to the analyzed flares. Hydrodynamic simulations and satellite data will complement the results to simulate the atmospheric response to the flare and compute the energy budget of the magnetic changes compared to other flare processes. The results will have a deep impact on flare models, future predictors, and space weather.


Net EU contribution
€ 160 932,48
38205 San Cristobal De La Laguna

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Canarias Canarias Tenerife
Activity type
Research Organisations
Total cost
€ 160 932,48