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Research Article
Table 3
Details on PROSPER’s peak flux fits for the SF bins, derived by equation (13). The filtering of the integral energy is first applied, and then there are three bins based on the magnitude of the solar flare. These fits are presented in Figure 9.
| If an event reaches E > 10 MeV | ||
|---|---|---|
| Flare flux < M3.0 |
M3.0 ≤ Flare flux < X1.0 |
Flare flux ≥ X1.0 |
| γ = 0.56 | γ = 0.40 | γ = 0.27 |
| x low = 2.63E+00 | x low = 2.97E+00 | x low = 7.69E+00 |
|
x
lim = 1.46E+03 |
x
lim = 1.17E+04 |
x
lim = 1.39E+04 |
| If an event reaches E > 30 MeV |
||
| Flare flux < M3.0 |
M3.0 ≤ Flare flux < X1.0 |
Flare flux ≥ X1.0 |
|
E > 10 MeV |
||
| γ = 0.52 | γ = 0.36 | γ = 0.28 |
| x low = 5.66E+00 | x low = 4.81E+00 | x low = 1.29E+01 |
|
x
lim = 1.36E+03 |
x
lim = 1.01E+04 |
x
lim = 1.43E+04 |
|
E > 30 MeV |
||
| γ = 0.76 | γ = 0.53 | γ = 0.28 |
| x low = 1.13E+00 | x low = 9.29E−01 | x low = 1.59E+00 |
|
x
lim = 3.27E+02 |
x
lim = 5.72E+03 |
x
lim = 2.29E+03 |
| If an event reaches E > 100 MeV |
||
| Flare flux < M3.0 |
M3.0 ≤ Flare flux < X1.0 |
Flare flux ≥ X1.0 |
|
E > 10 MeV |
||
| γ = 0.47 | γ = 0.27 | γ = 0.21 |
| x low = 7.74E+00 | x low = 1.06E+01 | x low = 2.66E+01 |
|
x
lim = 2.05E+04 |
x
lim = 9.42E+03 |
x
lim = 1.60E+04 |
|
E > 30 MeV |
||
| γ = 0.57 | γ = 0.3 | γ = 0.20 |
| x low = 1.91E+00 | x low = 2.74E+00 | x low = 5.33E+00 |
|
x
lim = 5.56E+02 |
x
lim = 2.52E+03 |
x
lim = 2.16E+03 |
|
E > 100 MeV |
||
| γ = 0.72 | γ = 0.53 | γ = 0.23 |
| x low = 3.67E−01 | x low = 3.33E−01 | x low = 7.12E−01 |
| x lim = 5.03E+00 | x lim = 1.88E+02 | x lim = 1.65E+02 |
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