An X2.0 and M9.4 flare from Active Region 13878 - October 31, 2024

  • Released Wednesday, November 27, 2024
View full credits

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 13878 presents a 'double whammy' of two strong flares (X 2.0 and M9.4) only about 30 minutes apart. For more details, see the Space Weather Database entries for X2.0 (peak @ 2024-10-31T21:20) and M9.4 (peak @ 2024-10-31T21:54).

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 some of this imagery.

Active Region 13878 (in the upper left quadrant of the disk) launches an X2.0 and M 9.4 flare in this view through the SDO AIA 131 ångstrom filter. PSF deconvolution has not been applied to these images to reduce the dark artifacting around the flare location.

Active Region 13878 (in the upper left quadrant of the disk) launches an X2.0 and M 9.4 flare in this view through the SDO AIA 171 ångstrom filter. PSF deconvolution has been applied to these images to improve the contrast of structures on the disk.

Active Region 13878 (in the upper left quadrant of the disk) launches an X2.0 and M 9.4 flare in this view through the SDO AIA 304 ångstrom filter. PSF deconvolution has been applied to these images to improve the contrast of structures on the disk.




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, November 27, 2024.
This page was last updated on Friday, November 22, 2024 at 8:46 AM EST.

Missions

This page is related to the following missions:

Series

This page can be found in the following series:

Datasets used

Note: While we identify the data sets used on this page, we do not store any further details, nor the data sets themselves on our site.