A Small (M5) Flare from Active Region 13078

  • Released Thursday, August 25, 2022
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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.

These movies were generated around a small M5 class solar flare that occurred on April 17, 2022 near the center of the lower hemisphere

The M5 solar flare (lower center of solar disk) as seen in AIA 171 Angstrom filter. Correction is applied for the instrument Point-Spread Function (PSF).


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.

Time-stamp slates for these frames.

Time-stamp slates for these frames.

Credits

Please give credit for this item to:
NASA's Scientific Visualization Studio

This page was originally published on Thursday, August 25, 2022.
This page was last updated on Wednesday, May 3, 2023 at 11:44 AM EDT.

Missions

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Datasets used in this visualization

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