Table 1.
Coronal-region filling factors from SaXS and image-based solar catalogs.
| Observation Date | Region Type | Coronal Filling Factors [%] | Notes | ||
|---|---|---|---|---|---|
| SaXS (this work) | HEKa | Hinode/XRTb | |||
| AR | 14.72 ± 23.67 | 19.91 | 7.66 (7.93 AR+XBP) | Flaring Sun DAXSS spectrum | |
| 2022 Apr. 25 | CO | 3.37 ± 0.22 | – | – | Not segmented in image databases |
| (Flaring Sun) | FL-AVG | 0.07 ± 0.0014 | 2.25 | – | Only from HEK bounding boxes |
| 2022 Jun. 29 | AR | 21.31 ± 5.76 | 8.06 | 4.02 | Quiescent Sun DAXSS spectrum |
| (Quiescent Sun) | BKC | 45.20 ± 149.53 | – | – | Not segmented in image databases |
Notes. Filling factors represent the fractional area of the solar disk within the solar limb (as defined by the Hinode/XRT segmentation maps) occupied by each coronal region. The SaXS filling factors are derived from spectral fits with variable abundances (Quiescent Sun) and variable abundances plus nonequilibrium ionization for the flare component (flaring Sun), as described in Sect. 3.3 using the XSPEC models VAPEC and VNEI, respectively. aHEK: bounding boxes of active regions and flares from multiple solar missions (Hurlburt et al. 2012). bHinode/XRT: segmentation maps of active regions and X-ray bright points from Adithya et al. (2021).
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