Table 2.
Onset times, inferred injection times and corresponding energies of SEPs observed by spacecraft, HXRs with various energies and electrons producing the radio bursts observed.
| Event | Onset time | Emission time | Energy | Method for |
|---|---|---|---|---|
| at spacecraft (UT) | at the Sun (UT) | injection time | ||
| Type II | 11:23 | 11:15 | – | – |
| Type III | 11:24 | 11:16 | – | – |
| Herringbones | 11:25 | 11:17 | 8 keV | – |
| Herringbones (solar equator) | 11:28 | 11:20 | 8 keV | – |
| HXR I | 11:20 | 11:12 | 25–50 keV | – |
| HXR II | 11:23 | 11:15 | 25–50 keV | – |
| Electrons (STA/SEPT) | 11:38 | 11:15 min |
45–55 keV | TSA |
| Electrons (STA/SEPT) | 11:34 | 11:21 min |
225–255 keV | TSA |
| Electrons (STA/HET) | 11:35 | 11:25 min |
0.7–1.4 MeV | TSA |
| Protons (STA/HET) | 11:51( * ) | 11:26 min |
13.6–100 (60–100*) MeV | VDA  AU |
| Electrons (Wind/3DP) | 11:47 | 11:22 min |
46.16–85.73 keV | TSA |
| Electrons (SOHO/EPHIN) | 11:46 | 11:33 min |
0.25–0.7 MeV | TSA |
| Protons (SOHO/ERNE) | 12:04( * ) | 11:40 min |
13–130 (64–80*) MeV | VDA  AU |
Notes. The method for determining the injection time is shown in the last column with the inferred propagation path length, L, in cases where VDA was used. The emission time at the Sun for particles is the injection time estimated using various methods presented in the last column. The emission time at the Sun in the case of the radio bursts and HXRs refers to the time when these radio bursts and HXRs are emitted taking into account the light-travel time to Earth of ∼8 min and 20 s. ( * ) Energy range of the first arriving particles at the spacecraft. This energy range is provided in brackets in the ‘Energy’ column also denoted by the * symbol.
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