Conditioning of the solar corona due to large flares

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Volume 695 (March 2025)

A&A, 695 (2025) A66

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Table 1.

Relative similarity of the pre-flare time evolution of photospheric and coronal quantities.

	ϕ_m	E	E_F	\|H_V\|	\|H_J\|
ϕ_m	×	0.53 ± 0.15	2.32 ± 0.59	3.03 ± 1.18	4.65 ± 1.51

E		×	1.77 ± 0.56	2.60 ± 1.06	4.11 ± 1.40

E_F			×	1.82 ± 0.64	2.57 ± 1.13

\|H_V\|				×	2.19 ± 0.61

\|H_J\|					×



	E_F/E₀		\|H_J\|/\|H_V\|		$\| H_{J} \| / {\tilde{ϕ}}^{2}$ $\|H_{\mathrm{J}}\|/\tilde\phi^2$

E_F/E₀	×		3.06 ± 1.40		2.52 ± 1.08

\|H_J\|/\|H_V\|			×		1.98 ± 0.77

$\| H_{J} \| / {\tilde{ϕ}}^{2}$ $\|H_{\mathrm{J}}\|/\tilde\phi^2$					×

Notes. Average values are computed from the cumulative costs of the flares of sample S_SEA. Uncertainties are defined based on the respective standard deviations. The cell colors are indicating the degree of similarity, and refer to ⟨C_cum⟩ ≤ 2.2 (dark red) as “highly similar”, 2.2 < ⟨C_cum⟩ ≤ 4.4 (orange) as “moderately similar”, and 4.4 < ⟨C_cum⟩ (light red) as “little similar”.

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