Table 1.
Relevant stellar parameters for our Hyades sample.
| RSP1 | Prot | D | L | M⋆ | R⋆ | Teff | RV | v sin i | ξt | ζt | i | τ | Ro | Ron |
|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|
| (d) | (pc) | (L⊙) | (M⊙) | (R⊙) | (K) | (m s−1) | (km s−1) | (°) | (d) | (–) | (–) | |||
| 344 | 5.14 | 45.147 | 1.63 | 1.20 | 1.155 | 6075 | 39 984 | 8.6 | 1.00 | 4.5 | 49 | 18.8 | 0.273 | 0.365 |
| 233 | 5.45 | 45.413 | 1.71 | 1.21 | 1.178 | 6088 | 38 754 | 9.8 | 1.00 | 4.5 | 64 | 18.2 | 0.299 | 0.400 |
| 340 | 5.87 | 46.993 | 1.90 | 1.22 | 1.213 | 6158 | 39 603 | 8.8 | 1.00 | 4.5 | 57 | 14.6 | 0.402 | 0.538 |
| 137 | 7.47 | 47.225 | 1.32 | 1.15 | 1.081 | 5954 | 37 942 | 6.2 | 0.95 | 4.3 | 58 | 24.4 | 0.306 | 0.409 |
| 177 | 8.38 | 45.467 | 0.98 | 1.10 | 0.995 | 5769 | 37 940 | 5.4 | 0.90 | 3.7 | 64 | 31.7 | 0.264 | 0.353 |
| 440 | 8.93 | 46.149 | 1.16 | 1.14 | 1.049 | 5856 | 40 815 | 5.4 | 0.95 | 4.0 | 65 | 28.5 | 0.313 | 0.419 |
| 227 | 8.96 | 46.749 | 0.70 | 1.05 | 0.899 | 5578 | 38 340 | 4.9 | 0.90 | 2.9 | 75 | 38.4 | 0.233 | 0.312 |
| 134 | 9.10 | 45.550 | 0.31 | 0.93 | 0.712 | 5125 | 37 294 | 3.7 | 0.85 | 1.9 | 69 | 53.4 | 0.170 | 0.227 |
| 439 | 9.16 | 52.093 | 0.30 | 0.92 | 0.717 | 5035 | 40 566 | 3.8 | 0.85 | 1.8 | 74 | 56.4 | 0.162 | 0.217 |
| 225 | 9.39 | 46.627 | 0.62 | 1.03 | 0.866 | 5517 | 39 158 | 3.9 | 0.90 | 2.6 | 57 | 40.4 | 0.232 | 0.310 |
| 95 | 9.82 | 40.735 | 0.34 | 0.98 | 0.750 | 5090 | 36 731 | 3.8 | 0.85 | 1.9 | 80 | 54.6 | 0.180 | 0.241 |
| 429 | 9.82 | 48.507 | 0.33 | 0.95 | 0.742 | 5103 | 40 578 | 3.8 | 0.85 | 1.9 | 84 | 54.1 | 0.182 | 0.243 |
| 198 | 10.26 | 50.824 | 0.45 | 1.00 | 0.796 | 5320 | 38 470 | 2.7 | 0.85 | 2.2 | 43 | 47.0 | 0.218 | 0.292 |
| 68 | 10.57 | 45.443 | 0.29 | 0.85 | 0.747 | 4916 | 31 328 | 2.7 | 0.85 | 1.6 | 49 | 60.5 | 0.175 | 0.234 |
| 587 | 11.79 | 50.718 | 0.16 | 0.83 | 0.613 | 4640 | 42 334 | 2.0 | 0.70 | 1.6 | 50 | 70.5 | 0.167 | 0.223 |
| 571 | 12.22 | 49.206 | 0.10 | 0.77 | 0.537 | 4446 | 41 902 | 2.2 | 0.70 | 1.6 | 82 | 80.4 | 0.152 | 0.203 |
| 216 | 12.64 | 44.958 | 0.25 | 0.88 | 0.699 | 4896 | 39 308 | 2.5 | 0.85 | 1.6 | 63 | 61.1 | 0.207 | 0.277 |
| 409 | 12.90 | 45.721 | 0.065 | 0.67 | 0.486 | 4191 | 40 887 | 1.7 | 0.70 | 1.6 | 63 | 97.8 | 0.132 | 0.177 |
| 133 | 13.51 | 47.174 | 0.048 | 0.63 | 0.438 | 4089 | 37 916 | 1.5 | 0.70 | 1.6 | 66 | 106 | 0.131 | 0.175 |
| 542 | 14.44 | 40.638 | 0.037 | 0.62 | 0.406 | 3994 | 42 379 | 1.4 | 0.70 | 1.6 | 80 | 118.5 | 0.122 | 0.163 |
| 556 | 15.99 | 48.159 | 0.019 | 0.59 | 0.327 | 3778 | 42 634 | 1.02 | 0.70 | 1.6 | 75 | 157 | 0.102 | 0.136 |
Notes. 1For other names, see Table C.1. 2The best-fit v sin i value is given, but we note that it is below the empirical lower limit of ≈1.3 km s−1. The distance, D, is from the Gaia DR3 parallax (Gaia Collaboration 2023) with the related luminosity, L, mass, M, and radius, R, all in solar units. Teff is the effective temperature from photometry. RV is the radial velocity from our spectra. v sin i is the projected rotational velocity from our spectra (errors are typically ±0.3 km s−1). The parameters ξt, ζt, and i denote the microturbulence, macroturbulence, and the inclination of the rotational axis, respectively. τ is the convective turnover time from Barnes & Kim (2010), Ro is the Rossby number Prot/τ, and Ron the normalized Rossby number (Ron, ⊙ = 1).
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