Table 1.
Younger main-sequence stars.
| Comparison | Spearman | Pearson | Kendall | Regression |
|---|---|---|---|---|
| Prot vs pcoupling | ρ = 0.269 | r = 0.257 | τ = 0.192 | R2 = 0.066 |
| (0.087–0.434) | (0.085–0.418) | (0.057–0.322) | RMSE = 7.417 | |
| p = 4.38 × 10−3 | p = 6.41 × 10−3 | p = 3.89 × 10−3 | MAE = 5.554 | |
| Prot vs pbcz | ρ = 0.208 | r = 0.175 | τ = 0.148 | R2 = 0.031 |
| (0.025–0.386) | (−0.019–0.388) | (0.009–0.276) | RMSE = 7.557 | |
| p = 2.88 × 10−2 | p = 6.54 × 10−2 | p = 2.57 × 10−2 | MAE = 5.490 | |
| Prot vs CCI | ρ = 0.345 | r = 0.250 | τ = 0.248 | R2 = 0.062 |
| (0.177–0.501) | (0.099–0.409) | (0.122–0.363) | RMSE = 7.432 | |
| p = 2.08 × 10−4 | p = 8.15 × 10−3 | p = 1.92 × 10−4 | MAE = 5.406 |
Notes. Correlation coefficients (Spearman’s ρ, Pearson’s r, and Kendall’s τ) and linear regression metrics for the relationship between stellar rotation period (Prot) and the percentile ranks for the depth of the convective zone and for the convective plasma parameter. Confidence intervals and p-values are provided for correlation coefficients.
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