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"title": "X2.7 and more flares from Active Region 14087 - May 14, 2025",
"description": "An X 2.7 flare from Active region 14087 and a couple more, May 14, 2025, as seen by Solar Dynamics Observatory (SDO).",
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"description": "Solar Dynamics Observatory (SDO) operates in a geosynchronous orbit around Earth to obtain a continuous view of the Sun. The particular instrument in this visualization records imagery in the ultraviolet portion of the spectrum at wavelengths normally absorbed by Earth's atmosphere - so we need to observe them from space.
\r\nAn X 2.7 flare an a couple others fire from Active region 14087 on May 14, 2025 as it comes over the left limb of the Sun. For more details, see the Space Weather Data entries for the M 5.3, X 2.7 and M 7.7 events
\r\nFor more information on the classification of solar flares, see Solar Flares: What Does It Take to Be X-Class? or X-Class: A Guide to Solar Flares. The point-spread function correction (PSF) has been applied to some of this imagery.",
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What is the PSF (Point Spread-Function)?
Many telescopes, especially reflecting telescopes such as the ones used on SDO (Wikipedia), have internal structures that support various optical components. These components can result in incoming light being scattered to other parts of the image. This can appear in the image as a faint haze, brightening dark areas and dimming bright areas. The point-spread function (Wikipedia) is a measure of how light that would normally be received by a single camera pixel, gets scattered onto other pixels. This is often seen as the \"spikes\" seen in images of bright stars. For SDO, it manifests as a double-X shape centered over a bright flare (see Sun Emits Third Solar Flare in Two Days). The effect of this scattered light can be computed, and removed, by a process called deconvolution (Wikipedia). This is often a very compute-intensive process which can be sped up by using a computers graphics-processing unit (GPU) for the computation.",
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