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Interface Region Imaging Spectrograph (IRIS) Observations of the Fractal Dimension in the Solar Atmosphere View all abstracts by submitter

Markus J. Aschwanden   Submitted: 2022-07-21 10:31

While previous work explored the fractality and self-organized criticality (SOC) of flares and nanoflares in wavelengths emitted in the solar corona (such as in hard X-rays, soft X-rays, and EUV wavelenghts), we focus here on impulsive phenomena in the photosphere and transition region, as observed with the Interface Region Imaging Spectrograph (IRIS) in the temperature range of Te ≈ 104-106 K. We find the following fractal dimensions (in increasing order): D_A=1.21 ± 0.07 for photospheric granulation, D_A=1.29 ± 0.15 for plages in the transition region, D_A=1.54 ± 0.16 for sunspots in the transition region, D_A=1.59 ± 0.08 for magnetograms in active regions, D_A=1.56 ± 0.08 for EUV nanoflares, D_A=1.76 ± 0.14 for large solar flares, and up to D_A=1.89 ± 0.05 for the largest X-class flares. We interpret low values of the fractal dimension (1.0 ≈ D_A ≈ 1.5) in terms of sparse curvi-linear flow patterns, while high values of the fractal dimension (1.5 ≈ D_A ≈ 2.0) indicate near space-filling transport processes, such as chromospheric evaporation. Phenomena in the solar transition region appear to be consistent with SOC models, based on their size distributions of fractal areas A and (radiative) energies E, which show power law slopes of α _Aobs=2.51 ± 0.21 (with α _Atheo=2.33 predicted), and α _Eobs=2.03 ± 0.18 (with α _Etheo=1.80 predicted).

Authors: Markus J. Aschwanden and Nived Vilangot Nhalil
Projects: None

Publication Status: Frontiers in Astronomy and Space Sciences (subm. 2022 Jul 21)
Last Modified: 2022-07-27 10:13
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