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Table 1

Sample of dM stars.

Star Year Sp. M ∗ R ∗ P rot Ro T eff log [L⋆/L⊙] [lin,lout] α0  (°) (G) (G)
ID obs. type (M⊙) (R⊙) (d) (0.01) (G) (K) (au) [Bp,0 = 1G] [Bp,0 = 1G] (au) [present] [young]
GJ 182 2007 M0.5 0.75 0.82 4.35 17.4 172 3950 − 0.88 [0.27,0.73] [4.0,7.7] [30,21] 1.3 [3.6,25] [0.28,2.0]
DT Vir 2008 M0.5 0.59 0.53 2.85 9.2 149 3790 − 1.26 [0.18,0.47] [5.5,11] [25,18] 0.48 [1.3,9.6] [0.11,0.75]
DS Leo 2008 M0 0.58 0.52 14.00 43.8 87 3770 − 1.29 [0.17,0.46] [5.9,11] [24,17] 0.44 [1.1,7.9] [0.086,0.62]
GJ 49 2007 M1.5 0.57 0.51 18.60 56.4 27 3750 − 1.31 [0.17,0.45] [6.1,12] [24,17] 0.42 [1.00,7.2] [0.078,0.56]
OT Ser 2008 M1.5 0.55 0.49 3.40 9.7 123 3690 − 1.38 [0.15,0.41] [3.7,7.1] [31,22] 0.81 [4.4,32] [0.35,2.5]
CE Boo 2008 M2.5 0.48 0.43 14.70 35.0 103 3570 − 1.56 [0.13,0.34] [3.0,5.8] [35,24] 0.90 [8.1,59] [0.63,4.6]
AD Leo 2008 M3 0.42 0.38 2.24 4.7 180 3540 − 1.67 [0.11,0.30] [2.5,4.9] [39,27] 1.0 [13,97] [1.0,7.6]
EQ Peg A 2006 M3.5 0.39 0.35 1.06 2.0 480 3530 − 1.73 [0.10,0.28] [2.2,4.2] [43,29] 1.2 [21,160] [1.7,12]
EV Lac 2007 M3.5 0.32 0.30 4.37 6.8 490 3480 − 1.88 [0.087,0.24] [1.9,3.8] [46,31] 1.2 [30,220] [2.4,17]
V374 Peg 2006 M4 0.28 0.28 0.45 0.6 640 3410 − 2.02 [0.074,0.20] [1.7,3.3] [50,34] 1.3 [45,340] [3.5,26]
EQ Peg B 2006 M4.5 0.25 0.25 0.40 0.5 450 3340 − 2.14 [0.065,0.18] [1.8,3.4] [49,33] 1.0 [39,290] [3.1,23]
GJ 1156 2009 M5 0.14 0.16 0.49 0.5 100 3160 − 2.60 [0.038,0.11] [3.3,6.5] [33,23] 0.23 [5.9,45] [0.46,3.5]
GJ 1245 B 2008 M5.5 0.12 0.14 0.71 0.7 60 3030 − 2.79 [0.031,0.085] [3.5,7.0] [32,22] 0.17 [4.8,37] [0.37,2.9]
WX UMa 2009 M6 0.10 0.12 0.78 0.8 1060 2770 − 3.10 [0.022,0.061] [1.0,1.7] [90,50] 1.0 [330,2600] [25,200]
DX Cnc 2009 M6 0.10 0.11 0.46 0.5 80 2700 − 3.19 [0.019,0.055] [2.8,5.5] [37,25] 0.16 [9.4,75] [0.73,5.9]

Notes. The columns are: the star name, the observation year, the stellar spectral type, mass M∗, radius R∗, rotation period Prot, Rossby number Ro, the average surface magnetic-field strength derived from the ZDI technique , effective temperature Teff, stellar bolometric luminosity L⋆, inner lin and outer lout edges of the insulation HZ, the upper limit of magnetospheric sizes rM (Eq. (4)) of planets with similar Earth’s magnetisation orbiting in the HZ and the corresponding aperture of their auroral ovals α0. is the closest orbital distance required for a terrestrial planet to sustain a present-day-Earth-sized magnetosphere (Eq. (9)). and are the range of the lowest planetary magnetic field (Eq. (10)) required for a terrestrial planet orbiting inside the HZ to sustain the present-day (11.7  rp) and young Earth’s (5  rp) magnetospheric size, respectively.

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