Characteristics and energy flux distributions of decayless transverse oscillations depending on coronal regions

Solar Orbiter First Results (Nominal Mission Phase)

Open Access

Table 3.

Linear Pearson correlation coefficients (CCs) between oscillation parameters as a function of the coronal region.

	σ	CC_P − L	CC_P − A	CC_P − D	CC_P − v	CC_P − F	CC_P − E	CC_L − A	CC_L − D	CC_L − v	CC_L − F	CC_L − E	CC_A − D	CC_A − v	CC_A − F	CC_A − E	CC_D − v	CC_D − F	CC_D − E	CC_v − F	CC_v − E	CC_F − E
AR	0.10	−0.14	0.38	0.88	−0.39	−0.86	−0.60	0.12	−0.15	0.24	0.35	0.37	0.18	0.52	0.27	0.52	−0.45	−0.83	−0.61	0.97	0.90	0.88
QS	0.08	0.26	0.20	0.86	−0.33	−0.85	−0.55	0.14	0.22	0.16	0.09	0.22	0.05	0.56	0.31	0.59	−0.33	−0.80	−0.52	0.97	0.91	0.87
ALL	0.06	0.02	0.28	0.87	−0.34	−0.84	−0.56	0.06	0.04	0.08	0.22	0.28	0.11	0.55	0.29	0.55	−0.37	−0.79	−0.53	0.96	0.89	0.88

Notes. The considered oscillation parameters are period (P), loop length (L), displacement amplitude (A), duration (D), velocity amplitude (v), energy flux (F), and energy (E). σ is the standard error ( $1 / \sqrt{n}$ $1/\sqrt{n}$ ), where n is the number of oscillations. The logarithmic scale is considered when calculating the correlation coefficient with the energy flux or energy.

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