Open Access
Table 1
The five main classes of SRBs which originate in the same of the solar atmosphere that are associated with geo-effective disturbances known as space weather (White, 2007; Yue et al., 2013).
| SRB | Description of spectrum | Duration | Frequency range | Associated origin mechanism |
|---|---|---|---|---|
| Type I | Short duration enhancements of narrow bandwidth usually appearing in groups. | A few seconds | 80–200 MHz | Active regions |
| Eruptive prominences | ||||
| Type II | Slow drift towards lower frequencies over the duration of the burst. Often accompanied by a harmonic. | 3–30 min | 20–150 MHz | MHD shocks |
| CMEs | ||||
| Proton emission events | ||||
| Flares | ||||
| Type III | Short duration. Quickest frequency drift rate of all metric radio bursts (White, 2007) | 1–3 s | 10 kHz–1 GHz | Active regions |
| Flares | ||||
| Type IV | Moving | 30 min – 2 h | 20–400 MHz | Flares, proton emissions |
| Stationary | Hours – days | 20 MHz–2 GHz | Eruptive prominences | |
| MHD shocks | ||||
| Continuum | 3–45 min | 25–200 MHz | Flares, proton emissions | |
| Type V | Always observed trailing a Type III burst. | 1–3 min | 10–200 MHz | Active regions, Flares |
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