Table 1.
Properties of the sample of stars used in this work.
| Name | Sp. type | M* | R* | d | LX | Prot | B0, low | Ṁlim,low | B0, high | Ṁlim,high |
|---|---|---|---|---|---|---|---|---|---|---|
| (M⊙) | (R⊙) | (pc) | (1028 erg s−1) | (d) | (G) | (Ṁ⊙) | (G) | (Ṁ⊙) | ||
| DO Cep | M4.0 | 0.316 | 0.332 | 4.0 | 0.23 | 0.41 | 150 | 50 | 1500 | 350 |
| WX UMa ( * ) | M6.0 | 0.095 | 0.121 | 4.9 | 0.36 | 0.78 | – | – | 4300 | 260 |
| AD Leo ( * ) | M3.0 | 0.42 | 0.431 | 4.97 | 3.2 | 2.23 | – | – | 1000 | 990 |
| GJ 625 | M1.5 | 0.317 | 0.332 | 6.47 | 0.04 | 79.8 ± 0.1 | 150 | 12 | 1500 | 140 |
| GJ 1151 ( * ) | M4.5 | 0.167 | 0.19 | 8.04 | 0.02 | 175.8 |
– | – | 150 | 9 |
| GJ 450 | M1.5 | 0.46 | 0.474 | 8.76 | 0.66 | 23 ± 1 | 110 | 80 | 1100 | 560 |
| LP 169−22 | M5.5 | 0.111 | 0.138 | 10.4 | < 0.03 | – | 320 | 75 | 3200 | 410 |
| CW UMa | M3.5 | 0.306 | 0.322 | 13.36 | 5.37 | 7.77 | 150 | 230 | 1500 | 1260 |
| HAT 182−00605 | M4.0 | 0.442 | 0.422 | 17.87 | 3.4 | 2.21 | 110 | 180 | 1100 | 1050 |
| LP 212−62 | M5.0 | 0.161 | 0.183 | 18.2 | 0.38 | 60.75 | 240 | 75 | 2400 | 410 |
| DG CVn ( † ) | M4.0 | 0.56 | 0.567 | 18.29 | 10.72 | 0.11 | 94 | 350 | 940 | 1900 |
| GJ 3861 | M2.5 | 0.419 | 0.43 | 18.47 | 3.36 | – | 120 | 200 | 1200 | 1120 |
| CR Dra ( † ) | M1.5 | 0.823 | 0.827 | 20.26 | 36.65 | 1.98 | 70 | 630 | 700 | 3400 |
| GJ 3729 ( † ) | M3.5 | 0.472 | 0.481 | 23.57 | 7.54 | 13.59 | 110 | 290 | 1100 | 1590 |
| G 240−45 | M4.0 | 0.125 | 0.162 | 27.59 | 0.02 | – | 300 | 22 | 3000 | 140 |
| 2MASS J09481615+5114518 | M4.5 | 0.122 | 0.161 | 36.17 | 0.28 | – | 300 | 76 | 3000 | 400 |
| LP 259−39 | M5.0 | 0.173 | 0.202 | 36.93 | 18.7 | – | 230 | 250 | 2300 | 1500 |
| 2MASS J10534129+5253040 | M4.0 | 0.408 | 0.379 | 45.19 | 28.01 | – | 120 | 370 | 1200 | 2160 |
| 2MASS J14333139+3417472 | M5.0 | 0.101 | 0.136 | 47.84 | 0.83 | – | 350 | 100 | 3500 | 540 |
Notes. For each star, we list the stellar mass M*, the stellar radius R*, the distance d, the X-ray luminosity LX, the rotation period Prot, the low estimate for the magnetic field strength B0, low and the corresponding mass-loss rate limit Ṁlim,low, and the high estimate for the magnetic field B0, high and its corresponding mass-loss rate limit Ṁlim,high. The systems marked with ( † ) are known close binary systems, for which we list the spectral type of the combined system. The stars marked with a ( * ) have magnetic field measurements from ZDI. The stellar properties are taken from Callingham et al. (2021b). The rotation period of GJ 1151 is taken from Lehmann et al. (2024).
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