The 8.2 μm mid-IR channel in solar flare footpoints peaks 0.3-0.45 s before the 5.2 μm channel due to wavelength-dependent opacity changes from flare-induced ionization.
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Reverberation lags in Mrk 817 range 3-8 days, exceed thin-disk models by factors of 3-6, follow a λ^{4/3} trend with the ICCF method, and vary by up to a factor of 2 between epochs.
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First time delay observation between two mid-infrared channels in solar flare footpoints
The 8.2 μm mid-IR channel in solar flare footpoints peaks 0.3-0.45 s before the 5.2 μm channel due to wavelength-dependent opacity changes from flare-induced ionization.
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AGN STORM 2. XII. Ground-Based Optical Photometry and Lag Measurements of Mrk 817
Reverberation lags in Mrk 817 range 3-8 days, exceed thin-disk models by factors of 3-6, follow a λ^{4/3} trend with the ICCF method, and vary by up to a factor of 2 between epochs.