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| Solarflare | |
|---|---|
| Name | Solarflare |
| Discovery | Ancient observations; modern spectroscopy |
| Field | Astrophysics, Heliophysics |
| Related | Sun, Solar cycle, Space weather |
Solarflare
A solar flare is a sudden, localized, intense release of electromagnetic energy from the atmosphere of the Sun associated with magnetic reconnection in active regions such as sunspot groups and active regions. Solar flares emit across the electromagnetic spectrum, from radio waves to gamma rays, and are closely linked to phenomena observed by missions like SOHO, Solar Dynamics Observatory, and Parker Solar Probe. Studies of flares connect work by researchers at institutions such as NASA, European Space Agency, and National Aeronautics and Space Administration-funded laboratories, and contribute to operational capabilities at agencies like NOAA and the European Space Agency's Space Weather programs.
Solar flares occur when stored magnetic energy in the Sun's atmosphere is rapidly converted into particle acceleration, heating, and radiation, producing signatures observed by observatories including Hinode, IRIS, and ground-based facilities like the Big Bear Solar Observatory. They are studied within the context of the 11-year solar cycle modulation of activity and of structures such as coronal loops, active regions, and magnetic reconnection sites documented by teams at Harvard–Smithsonian Center for Astrophysics and Lockheed Martin Solar and Astrophysics Laboratory. Flares are categorized by intensity and morphology and are central to the discipline of heliophysics and to operational space weather forecasting by agencies such as NOAA's Space Weather Prediction Center.
Magnetic reconnection in the corona and at the interface with the chromosphere underpins current models, drawing on theoretical frameworks developed by researchers at Princeton University and Stanford University and numerical simulations run on facilities like NAS resources. Flares involve conversion of magnetic free energy into kinetic energy of electrons and ions, radiation, and bulk plasma motions observed as coronal mass ejections or confined to flare loops; mechanisms have been explored in papers from groups at Max Planck Institute for Solar System Research and University of Tokyo. Particle acceleration processes link to studies of solar energetic particles and to observational campaigns by instruments on RHESSI, Fermi Gamma-ray Space Telescope, and WIND.
Flares are classified by soft X-ray peak flux using the system employed by NOAA and the GOES satellite series into classes (A, B, C, M, X) with sublevels; this operational taxonomy is used by operators at NOAA Space Weather Prediction Center and by analysts at European Space Agency. Morphological classifications include compact versus two-ribbon flares studied by teams at Kwasan Observatory and historic catalogs maintained by National Solar Observatory. Characteristic timescales range from minutes to hours; associated radiative outputs affect spectral bands monitored by STEREO, Hinode, and the Atmospheric Imaging Assembly on SDO.
Observations use multiwavelength instrumentation: X-ray photometers on GOES, imaging spectrometers on RHESSI, EUV imagers on SDO/AIA, radio arrays such as Nobeyama Radioheliograph and LOFAR, and coronagraphs on SOHO/LASCO and STEREO spacecraft. Ground-based spectroscopy with facilities like McMath–Pierce Solar Telescope and polarimetric measurements at Dunn Solar Telescope probe magnetic topology; data assimilation efforts involve groups at European Centre for Medium-Range Weather Forecasts-partnered research and the Community Coordinated Modeling Center. Machine learning and data-driven methods from teams at Google and university labs augment event detection and classification.
Large flares can produce enhanced fluxes of solar energetic particles that perturb planetary magnetospheres such as Earth's magnetosphere and ionosphere, impact Mars's atmosphere observed by MAVEN, and affect spacecraft operations for missions like Voyager and Juno. Coupling with coronal mass ejections can trigger geomagnetic storms measured by indices used by NOAA and World Meteorological Organization-affiliated services; terrestrial impacts include radio blackouts observed by Federal Communications Commission-regulated services, satellite surface charging studied by European Space Agency engineers, and increased drag on low Earth orbit assets monitored by United States Space Force units.
Operational forecast centers including NOAA Space Weather Prediction Center and the Met Office use observations from SDO, SOHO, and ground networks to issue alerts; models include physics-based ensembles from groups at Predictive Science Inc. and empirical methods developed at University of Colorado Boulder. Modern efforts combine helioseismology results from GONG and synoptic magnetograms from SOLIS with machine learning frameworks from academic consortia at Stanford University and MIT to improve flare probability forecasts and nowcasting used by satellite operators and aviation regulators like International Civil Aviation Organization.
Notable flares and associated disturbances include the 1859 event observed by Richard Carrington and Richard Hodgson that produced the Carrington Event aurorae and telegraph disruptions; the 1989 geomagnetic storm that caused power outages in Quebec and involved analysis by Hydro-Québec engineers; the series of events during the solar maximum of 2003 ("Halloween storms") that affected missions like Aerospace Corporation-supported satellites; and intense episodes monitored during the approaches of Ulysses, SOHO, and Parker Solar Probe that have been the subject of studies at Jet Propulsion Laboratory. These events shaped policy and technical responses at organizations such as NOAA, NASA, and national infrastructure agencies.