Table 1
Parameters retrieved from the literature for the stars in our sample.
| Star | Gliese ID | Spectral type | Prot (d) | M (M⊙) | R (R⊙) | τ (d) | RO |
|---|---|---|---|---|---|---|---|
| DS Leo | Gl 410 | M1.0V | 14.0 ± 0.11 | 0.57 ± 0.02 | 0.53 ± 0.02 | 38 ± 23 | 0.37 ± 0.23 |
| AD Leo | Gl 388 | M3V | 2.2399 ± 0.00062 | 0.42 ± 0.02 | 0.39 ± 0.02 | 57 ± 33 | 0.04 ± 0.02 |
| EV Lac | Gl 873 | M4.0V | 4.3715 ± 0.00062 | 0.32 ± 0.02 | 0.31 ± 0.02 | 76 ± 42 | 0.06 ± 0.03 |
| Barnard’s star | Gl 699 | M4V | 136 ± 133 | 0.16 ± 0.02 | 0.185 ± 0.004 | 125 ± 67 | 1.09 ± 0.59 |
| PM J18482+0741 | ... | M5.0V | 2.76 ± 0.014 | 0.14 ± 0.02 | 0.17 ± 0.02 | 134 ± 71 | 0.02 ± 0.01 |
| CN Leo | Gl 406 | M6V | 2.704 ± 0.0034 | 0.11 ± 0.02 | 0.13 ± 0.02 | 147 ± 79 | 0.02 ± 0.01 |
Notes. Masses and radii were taken from Cristofari et al. (2023a,b). Convective turnover times (τ) were computed from the mass using the relation introduced in Wright et al. (2018). The Rossby number is defined as R0 = Prot/τ. References: (1) Donati et al. (2008), (2) Morin et al. (2008), (3) Donati et al. (2023b), (4) Díez Alonso et al. (2019).
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