Table A.1.
Summary of solar flare composition measurements
| Author and paper | FIP bias | Element or Diagnostic | Class (no. of flares) | Instruments |
|---|---|---|---|---|
| Veck & Parkinson (1981) | photospheric | Ca, Si, S, and Ar | N/A (10) | OSO-8 |
| Feldman & Widing (1990) | photospheric | O/Mg, Ne/Mg, | M1 (1) | Skylab spectroheliograms |
| and Ar/Mg | ||||
| Fludra & Schmelz (1995) | photospheric | Mg, Si, S, Ne, and O | M5 (1) | SMM/BCS |
| Bentley et al. (1997) | photospheric | Ca | N/A (177) | Yohkoh/BCS |
| Fludra & Schmelz (1999) | photospheric | Ca, Fe, and S | N/A (57) | Yohkoh/BCS |
| Phillips et al. (2003) | photospheric | S, and Ar | M5.5, M9 (2) | CORONAS-F/RESIK |
| Sylwester et al. (2012) | photospheric | S | C3.4–M4.9 (13) | CORONAS-F/RESIK |
| Del Zanna & Woods (2013) | photospheric | Ca/Fe and Ar/Fe | X5.6 (1) | SDO/EVE |
| Sylwester et al. (2014) | photospheric | Si, S, and Ar | M1 (1) | CORONAS-F/RESIK |
| Warren (2014) | photospheric | Fe | M9.3–X6.9 (21) | SDO/EVE |
| Narendranath et al. (2014) | photospheric | S, and Ar | C2.8 (1) | Chandrayaan-1/XSM |
| Dennis et al. (2015) | photospheric | Fe, Si and S | N/A* (526) | MESSENGER/SAX |
| Sylwester et al. (2015) | photospheric | S, and Ar | B9.9–X1.5 (33) | CORONAS-F/RESIK |
| Katsuda et al. (2020) | photospheric | Si, S, and Ar | X5.4–17.0 (4) | Suzaku/XIS |
| Narendranath et al. (2020) | photospheric | Ca, Fe, Si, and S | A3–M4 (44) | SMART-1, |
| Chandrayaan-1/XSM, | ||||
| and MESSENGER/SAX | ||||
| Mondal et al. (2021) | photospheric | Al, Mg, and Si | B1.3–4.5 (9) | Chandrayaan-2/XSM |
| Sylwester et al. (2022) | photospheric | Si, S, and Ar | B6.4–X13 (194) | SMM/BCS |
| Mithun et al. (2022) | photospheric | Mg, Fe, and Si | C1.6–5.7 (3) | Chandrayaan-2/XSM |
| Nama et al. (2023) | photospheric | Al, Mg, Si, and S | A1.1–3.4 (17) | Chandrayaan-2/XSM |
| Rao et al. (2023) | photospheric | Mg, Si, S | B1.8 (1) | Chandrayaan-2/XSM |
| Kępa et al. (2023) | photospheric | Ca, Mg, Fe, Si, and S | M3.9 (1) | Chandrayaan-2/XSM |
| Telikicherla et al. (2024) | photospheric | Ca, Mg, Fe, Si, and S | C2.5–M2.7 (6) | MinXSS/DAXSS |
| Sylwester et al. (1984) | weakly fractionated | Ca | N/A | SMM/BCS |
| Doschek et al. (1985) | weakly fractionated | K, Ca, and Ar | N/A | SOLFLEX |
| Schmelz (1993) | weakly fractionated | S, and Ne | M1.5, M5 (2) | SMM/FCS |
| Sterling et al. (1993) | weakly fractionated | Ca | M1–X2 (25) | SOLFLEX |
| Fludra & Schmelz (1995) | weakly fractionated | Ca | M5 (1) | SMM/BCS |
| Sylwester et al. (1998) | weakly fractionated | Ca | C1.9–X1.1 (138) | SMM/BCS |
| Sylwester et al. (2011) | weakly fractionated | Cl | C1–X1 (20) | CORONAS-F/RESIK |
| Phillips & Dennis (2012) | weakly fractionated | Fe | M1.6–X8.3 (20) | RHESSI |
| Narendranath et al. (2014) | weakly fractionated | Si | C2.8 (1) | Chandrayaan-1/XSM |
| Dennis et al. (2015) | weakly fractionated | Ar | N/A* (526) | MESSENGER/SAX |
| Katsuda et al. (2020) | weakly fractionated | Ca | X5.4–17.0 (4) | Suzaku/XIS |
| Nama et al. (2023) | weakly fractionated | Al | A1.1–3.4 (17) | Chandrayaan-2/XSM |
| Sylwester et al. (2023) | weakly fractionated | Ca | B–X (194) | SMM/BCS |
| Suarez & Moore (2023) | weakly fractionated | Fe, Si, S, and Ar | C1.2–M7.6 (21) | MinXSS-1 |
| Kępa et al. (2023) | weakly fractionated | Al | M3.9 (1) | Chandrayaan-2/XSM |
| Phillips et al. (2003) | coronal | K | M5.5, M9 (2) | CORONAS-F/RESIK |
| Sylwester et al. (2006) | coronal | K | N/A (1163) | CORONAS-F/RESIK |
| Dennis et al. (2015) | coronal | Ca | N/A* (526) | MESSENGER/SAX |
| Narendranath et al. (2014) | coronal | Ca, and Fe | C2.8 (1) | Chandrayaan-1/XSM |
| Sylwester et al. (2015) | coronal | K | B9.9–X1.5 (33) | CORONAS-F/RESIK |
| Sylwester et al. (2022) | coronal | Ca, and Fe | B6.4–X13 (194) | SMM/BCS |
| Suarez & Moore (2023) | coronal | Ca | C1.2–M7.6 (21) | MinXSS-1 |
Notes. Sun-as-a-star or non-spatially resolved FIP bias measurements in solar flares, during the peak phase of flares, sorted by the qualitative description of the FIP bias (photospheric, weakly fractionated, and coronal). Photospheric: FIP bias values ∼1; Weakly fractionated: FIP bias values ∼2; Coronal: FIP bias > 3. The table includes information on the observed elements, instruments used, and references for each study. Most instruments observe in the X-ray wavelength range, with the exception of Skylab spectroheliograms and SDO/EVE, which operate in the extreme-ultraviolet (EUV) range. It is important to note that some studies investigated the FIP bias of multiple flares, and the quoted FIP bias values represent their average measurements. Additionally, certain studies found substantial flare-to-flare variations in the composition measured. First Ionization Potential (FIP) values for relevant elements: K (4.34 eV), Al (5.99 eV), Ca (6.11 eV), Mg (7.65 eV), Fe (7.90 eV), Si (8.15 eV), S (10.36 eV), Cl (12.97 eV), O (13.62 eV), Ar (15.76 eV), Ne (21.56 eV). *Dennis et al. (2015) mentioned large flare, but no details on the flare class.
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