Solar phenomena

Solar phenomena are observable events and structures associated with the Sun, including changes in its magnetic field, atmosphere, and emitted radiation.

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Solar magnetic field: The magnetic field generated by moving plasma inside the Sun and extending through its atmosphere and interplanetary space. Its changing structure drives many active regions and eruptions.
Sunspot: A relatively cool, dark region of the photosphere associated with concentrated magnetic fields. Sunspots mark magnetic concentrations where active regions develop.
Space weather: Conditions in space influenced by the Sun and solar wind that can affect Earth and technological systems. Solar eruptions are major drivers of changing space-weather conditions.
Solar filament: A relatively cool, dense strand of solar plasma seen as a dark feature against the bright solar disk. Filaments are prominences viewed against the solar disk.
Solar atmosphere: The Sun’s outer gaseous layers: the photosphere, chromosphere, and corona. Different phenomena appear in distinct atmospheric layers.
Solar flare: A sudden, intense release of energy from the Sun’s atmosphere, producing radiation across the electromagnetic spectrum. Flares convert stored magnetic energy into radiation and accelerated particles.
Geomagnetic storm: A disturbance of Earth’s magnetosphere caused by energy and particles from the solar wind. Earth-directed coronal mass ejections can trigger severe storms.
Solar granule: A small, short-lived cellular pattern on the photosphere produced by convection beneath it. Granules arise from surface convection, unlike magnetically driven active phenomena.
Photosphere: The visible layer of the Sun from which most sunlight escapes. Sunspots are dark features observed against this layer.
Solar prominence: A large, dense structure of plasma suspended in the solar corona by magnetic fields. Its magnetic support can become unstable before an eruption.