Table 2
Details of model runs.
| Run | Star | Spectrum | Spectrum | Planet | a | Rotational |
| # | quiescent | flare | [AU] | period | ||
|
|
||||||
| 1 | HD 189733 | ϵ Eri quiet | ϵ Eri quiet + scaled Sun flare | HD 189733b | 0.031 | Phase locked |
| 2 | HD 189733 | ϵ Eri quiet | ϵ Eri quiet + scaled AU Mic flare | HD 189733b | 0.031 | Phase locked |
| 3 | HD 209458 | Sun quiet | Sun flare | HD 209458b | 0.047 | Phase locked |
| 4 | AU Mic | AU Mic quiet | AU Mic flare | HD 209458b | 0.2 | Phase locked |
| 5 | AU Mic | AU Mic quiet | AU Mic flare | HD 209458b | 1.0 | 10 h |
Notes. Numbers are used to identify each run (#) and parameters of the star and planet modelled are provided. The flaring spectra for runs #1 and #2 are made up of the quiet spectrum for ϵ Eri (proxy for HD 189733) onto which is added the flare excess energy of either a solar flare (#1) or a flare on AU Mic (#2), scaled according to X-ray observations of flares on HD 189733 (see text for more details). In the cases where the planet is phase locked with its star, the rotational period is synchronised to the planet’s orbital period.
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