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Table A.1

Stellar parameters and abundances derived in the sample of M dwarfs.

Karmn Name Teff (K) log g C/O [M/H] log ɛ(Rb) log ɛ(Sr) log ɛ(Zr)
J00051+457 GJ 2 3772 4.68 0.59 0.10 2.32 ± 0.02 2.91 2.70
J00183+440 GX And 3606 4.77 0.61 − 0.14 2.12 ± 0.05 2.58 2.50
J00389+306 G 60–10 3491 4.78 0.59 −0.10 2.22 ± 0.01 2.73 2.55
J00570+450 G 172–30 3397 4.85 0.50 −0.10 2.13 ± 0.01 2.90 2.80
J01013+613 GJ 47 3496 4.80 ... −0.11 2.00 ± 0.02 2.80 2.55 ± 0.02
J01025+716 GJ 48 3432 4.78 0.47 0.00 2.19 ± 0.01 2.85 2.60
J01026+623 BD+61 195 3810 4.67 0.54 0.06 2.45 2.98 2.63
J01433+043 G 3–14 3485 4.80 0.50 −0.10 1.99 ± 0.03 2.70 2.60 ± 0.01
J01518+644 G 244–37 3666 4.64 0.58 0.20 2.42 ± 0.02 2.96 2.72 ± 0.02
J02015+637 G 244–47 3452 4.79 0.59 0.03 2.44 ± 0.01 2.90 2.61 ± 0.01
J02123+035 BD+02 348 3605 4.90 0.58 −0.35 1.80 ± 0.02 2.57 2.45 ± 0.03
J02222+478 BD+47 612 3916 4.64 0.58 0.15 2.43 ± 0.02 2.95 2.70 ± 0.01
J02358+202 BD+19 381 3726 4.63 0.59 0.18 2.48 ± 0.03 2.93 2.60 ± 0.01
J02442+255 G 36–31 3434 4.83 0.58 0.00 2.12 ± 0.02 2.98 2.63 ± 0.01
J02565+554W G 174–19 3889 4.64 0.54 0.30 2.54 ± 0.02 2.98 2.73 ± 0.01
J03181+382 BD+37 748 3854 4.64 0.58 0.20 2.72 ± 0.01 3.20 2.83 ± 0.02
J03213+799 GJ 133 3533 4.78 0.59 −0.10 2.05 ± 0.05 ... 2.50 ± 0.01
J03217−066 G 77–46 3502 4.85 0.54 −0.10 1.99 ± 0.04 2.98 2.65 ± 0.02
J03463+262 HD 23453 4001 4.66 0.54 0.20 2.40 ± 0.05 3.11 2.78 ± 0.02
J03531+625 Ross 567 3454 4.79 0.59 −0.05 2.00 ± 0.02 2.65 2.48 ± 0.01
J04225+105 LSPM J0422+1031 3415 4.80 ... 0.05 2.55 ± 0.01 2.89 2.73
J04290+219 HD 28343 4187 4.63 0.54 0.30 2.65 ± 0.01 3.17 2.85 ± 0.05
J04376−110 BD−11 916 3611 4.74 0.59 0.05 2.12 ± 0.05 2.93 2.70 ± 0.01
J04376+528 HD 232979 4010 4.64 0.58 0.00 2.10 ± 0.05 2.92 2.63 ± 0.01
J04429+189 HD 285968 3689 4.66 0.58 0.12 2.54 ± 0.01 2.85 2.60 ± 0.01
J04538−177 L 736-30 3543 4.76 0.58 −0.10 2.06 ± 0.01 2.60 2.50 ± 0.01
J04588+498 BD+49 1280 4004 4.64 0.52 0.15 2.36 ± 0.03 3.00 2.79 ± 0.04
J05127+196 GJ 192 3570 4.75 0.54 −0.01 2.19 ± 0.02 2.87 2.78 ± 0.02
J05314−036 HD 36395 3700 4.95 0.67 0.25 2.70 ± 0.02 3.40 2.97 ± 0.02
J05365+113 HD 245409 4062 4.66 0.43 0.05 2.24 ± 0.03 3.05 2.79 ± 0.01
J05415+534 HD 233153 3869 4.63 0.63 0.15 2.38 ± 0.02 3.00 2.82 ± 0.02
J06103+821 GJ 226 3500 4.90 0.57 −0.05 2.07 ± 0.02 2.85 2.65 ± 0.05
J06105−218 HD 42581 3842 4.68 0.54 0.10 2.43 ± 0.02 2.90 2.66 ± 0.03
J06371+175 Ross 85 3732 4.77 0.63 −0.25 1.83 ± 0.02 2.40 2.37
J06548+332 Wolf 294 3410 4.85 0.57 0.00 2.28 ± 0.05 2.87 2.62 ± 0.01
J07044+682 GJ 258 3421 4.81 0.57 0.05 2.32 ± 0.01 2.90 2.65 ± 0.01
J07287−032 GJ 1097 3420 4.81 0.58 0.01 2.30 ± 0.02 2.83 2.63 ± 0.02
J07353+548 GJ 3452 3513 4.81 0.59 −0.05 2.08 ± 0.01 2.70 2.63 ± 0.01
J07361−031 BD−02 2198 3790 4.70 ... −0.04 2.05 ± 0.02 2.60 2.59 ± 0.02
J08161+013 G 113–0 3534 4.77 0.57 −0.04 2.15 ± 0.01 2.60 2.60 ± 0.01
J08293+039 2M J08292191+0355092 3685 4.64 0.54 0.22 2.52 ± 0.01 2.88 2.63 ± 0.01
J08358+680 G 234–37 3434 4.82 0.57 −0.06 2.05 ± 0.01 2.85 2.64 ± 0.03
J09133+688 G 234–57 3494 4.86 ... −0.05 2.00 ± 0.05 2.98 2.70 ± 0.05
J09140+196 LP 427–16 3591 4.65 0.58 0.11 2.20 ± 0.05 2.95 2.59 ± 0.01
J09143+526 HD 79210 4007 4.67 0.58 0.07 2.17 ± 0.02 2.97 2.68 ± 0.01
J09144+526 HD 79211 3980 4.67 0.49 0.10 2.17 ± 0.01 2.95 2.71 ± 0.02
J09163−186 L 749–34 3524 4.85 0.57 −0.12 1.97 ± 0.01 2.89 2.72 ± 0.02
J09411+132 Ross 85 3654 4.72 0.57 0.03 2.19 ± 0.02 2.90 2.65 ± 0.01
J09425+700 GJ 360 3718 4.67 0.41 0.10 2.55 ± 0.02 2.80 2.80
J11054+435 BD+44 2051A 3617 4.79 0.43 −0.20 2.05 ± 0.02 2.80 2.53
J11201−104(a) LP 733–099 3469 4.91 0.58 −0.20 1.78 ± 0.02 2.57 2.50 ± 0.01
J12111−199 LTT 4562 3440 4.83 0.59 −0.10 2.18 ± 0.02 2.75 2.70
J13450+176 BD+18 2776 3900 4.80 0.57 −0.50 1.75 ± 0.05 2.30 2.20
J13457+148 HD 119850 3610 4.73 0.47 −0.10 2.12 ± 0.02 2.58 2.65
J15218+209(a) OT Ser 3500 4.90 0.58 0.10 2.05 2.71 2.70 ± 0.02
J18174+483(a) TYC 3529-1437-1 3435 4.80 0.59 −0.08 1.85 ± 0.02 2.88 2.58 ± 0.01
J22565+165 HD 216899 3606 4.77 0.59 0.15 2.55 ± 0.01 3.02 2.75

Notes. The C/O ratio in the Sun is 0.575 (Lodders 2019). Abundances of Rb, Sr, and Zr are given on the scale log N(H) ≡ 12. The Sr abundances shown are corrected for non-LTE effects (see text). For Rb and Zr abundances, the abundance dispersion is also tabulated. (a) The resonance Rb lines in these stars may be affected by magnetic field. Their abundance ratios are indicated as red open circles in Figs. 5 and 8.

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