Table 2
Comparison of potential emission mechanisms with key observational and physical constraints.
| Mechanism | Power | fce | fpe/ fce | Viewing angle |
|---|---|---|---|---|
| Sub-Alfvénic SPI | Yes | Yes | Plausible (hotspot)† | Marginal‡ |
| Wind-magnetosphere | Plausible | Unknown | Unknown | Favorable‡ |
| Stellar CMI | Yes | Yes | Plausible (hotspot)† | Irrelevant |
| Stellar plasma emission | Plausible (flare) | Irrelevant | Irrelevant | Irrelevant |
Notes. (†) A low fpe/ fce ratio is required for CMI to operate. In dense stellar coronae, this ratio is typically too high unless conditions are locally altered (e.g., magnetic hotspots). (‡) The fact that the burst was detected during the exoplanet’s transit rather than in quadrature supports the wind-magnetosphere rather than the sub-Alfvenic SPI model.
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