Solar X-Flare - October 2, 2022 (X1.0 class)

  • Released Friday, October 21, 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.

Here we have multi-wavelength views of an X1.0 class flare from early October 2022 (upper right of image). Solar flares are classified by the amount of energy released (Solar Flares: What Does It Take to Be X-Class?). Several long filaments or prominences (the dark ribbons) meander across the lower hemisphere.

The solar flare as seen in AIA 131 Angstrom filter. Correction is applied for the instrument Point-Spread Function (PSF). The dark area around the flare event is an artifact of the point-spread function correction process.


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

The solar flare as seen in AIA 304 Angstrom filter. Correction is applied for the instrument Point-Spread Function (PSF).

Time-stamp slates for these frames, organized by wavelength.

Time-stamp slates for these frames, organized by wavelength.


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.

For More Information

See NASA.gov

Credits

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

This page was originally published on Friday, October 21, 2022.
This page was last updated on Wednesday, May 3, 2023 at 11:43 AM EDT.

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