An X1.7 flare from Active Region 13765 and some extra energetic activity - August 5, 2024

  • Released Wednesday, October 2, 2024
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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 AR 13765 launches an X1.7 flare on August 5, 2024 on the rightmost part of the solar limb. Shortly thereafter, an X1.1 flare launches near the left limb from AR 13780. For more details, see the Space Weather Database entry for X1.7 and X1.1. Towards the end of this visualization, around 18:35 TAI, a bright filament launches near the center of the disk.

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 13765 (near the right limb of the disk) launches an X1.7 flare followed by AR 13780 launching an X1.1 flare (near the left limb), in this view through the SDO AIA 131 ångstrom filter. Later, a bright filament launches from a region near the center of the disk.

Active Region 13765 (near the right limb of the disk) launches an X1.7 flare followed by AR 13780 launching an X1.1 flare (near the left limb), in this view through the SDO AIA 171 ångstrom filter. Later, a bright filament launches from a region near the center of the disk.

Active Region 13765 (near the right limb of the disk) launches an X1.7 flare followed by AR 13780 launching an X1.1 flare (near the left limb), in this view through the SDO AIA 304 ångstrom filter. Later, a bright filament launches from a region near the center of 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.
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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.

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NASA's Scientific Visualization Studio

This page was originally published on Wednesday, October 2, 2024.
This page was last updated on Wednesday, October 2, 2024 at 3:01 PM EDT.

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