M 8.2 flare at Active Region 13435 - September 20, 2023

  • Released Wednesday, December 13, 2023
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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.

Active Region 13435 near the solar equator erupts with an M8.2 flare as it approaches the center of the solar disk. A second similar event will erupt the next day. For details of this event, see the Space Weather database entry.

For 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 all this imagery.


Active Region AR13435 launches an M8.2 flare as it approaches the center of the solar disk in this view from the SDO/AIA 131A filter. It will erupt again the next day. The point-spread function correction (PSF) has been applied to all this imagery.

Active Region AR13435 launches an M8.2 flare as it approaches the center of the solar disk in this view from the SDO/AIA 171A filter. It will erupt again the next day. The point-spread function correction (PSF) has been applied to all this imagery.

Active Region AR13435 launches an M8.2 flare as it approaches the center of the solar disk in this view from the SDO/AIA 304A filter. It will erupt again the next day. The point-spread function correction (PSF) has been applied to all this imagery.


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 slates for the multiple movies above, for custom compositing. Make sure to match the event and frame tag for the SDO frames you are using.

Time slates for the multiple movies above, for custom compositing. Make sure to match the event and frame tag for the SDO frames you are using.

Credits

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

This page was originally published on Wednesday, December 13, 2023.
This page was last updated on Tuesday, December 12, 2023 at 1:32 PM EST.

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