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Table 2.

Number of stars of different spectral types in the tidal tail at the Pleiades age (i.e. t = 125 Myr).

Run name Ntl Ntl, π/4 NA, tl NF, tl NG, tl NK, tl fA, tl fF, tl fG, tl fK, tl
C03G13 2437 971 53 91 101 217 0.022 0.037 0.042 0.090 2.69 3.85 4.03
C03G23 453 266 9 15 17 35 0.021 0.035 0.038 0.079 0.15 0.15 0.15
C03GA 147 96 3 5 5 13 0.022 0.037 0.037 0.090 0.07 0.07 0.07
C03W1 109 79 2 3 3 7 0.015 0.026 0.031 0.068 0.02 0.02 0.03
C03W5 607 524 13 24 24 54 0.022 0.039 0.041 0.091 0.23 0.25 0.24
C10G13 6116 1712 133 234 272 550 0.022 0.038 0.045 0.091 1.42 1.52 1.55
C10G23 926 413 18 31 36 67 0.020 0.034 0.041 0.075 0.08 0.08 0.08
C10GA 328 167 4 7 12 20 0.012 0.024 0.038 0.068 0.02 0.02 0.02
C10W1 173 94 0 3 4 11 0.000 0.018 0.025 0.074 0.00 0.01 0.01
C10W5 478 341 9 16 22 41 0.019 0.036 0.049 0.090 0.04 0.05 0.05

Notes. From left to right, the columns list model name; total number of stars in the tidal tail Ntl; total number of tail stars Ntl, π/4 angularly closer than 45° to the cluster, as seen from the Solar System; number NC, tl of stars of spectral class C (where C stands for A, F, G, and K) in the tidal tail; number fraction fC, tl of stars of spectral class C in the tidal tail (e.g. fA, tl = NA, tl/Ntl). The canonical IMF (Kroupa 2001) populated from 0.08 M⊙ to 120 M⊙ results in number fractions of fA = 0.028, fF = 0.038, fG = 0.041, and fK = 0.101. We also compare the ratio of the tail NC, tl to cluster NC, cl population for stars of spectral types A, F, and FGK together. The table is a result of all realisations of the models; for example, NA, tl = 2 for model C03W1 is an average of 13 models containing 26 A stars.

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