Table 4.

Simulated present-day properties (mean values between ages of 620 and 695 Myr for M1, M2 and M3 and 615 to 635 Myr for M4; time before cluster disruption) of the Hyades star cluster.

Parameter Value – M1 Value – M2 Value – M3 Value – M4( ⋆ ) Value – M4( † ) Value – M5
, lumps , lumps
(during disruption)
Rt [pc] 9.2 ± 0.1 9.5 ± 0.1 7.9 ± 0.1 5.2 ± 0.2 4.9 ± 0.7 9.1 ± 0.1
σ(r < Rt) [km s−1] 0.55 ± 0.01 0.57 ± 0.02 0.53 ± 0.01 0.85 ± 0.07 0.95 ± 0.09 0.52 ± 0.01
σ(r < 3 pc) [km s−1] 0.62 ± 0.01 0.68 ± 0.02 0.66 ± 0.05 1.2 ± 0.1 1.17 ± 0.06 0.61 ± 0.01
σ(r < 9 pc) [km s−1] 0.55 ± 0.01 0.58 0.01 0.52 ± 0.01 0.68 ± 0.02 0.93 ± 0.27 0.53 ± 0.01
M(r < Rt) 394 ± 11 436 ± 6 249 ± 2 60 ± 5 56 ± 2 380 ± 7
M(r < 30 pc) 536 ± 7 568 ± 4 423 ± 8 191 ± 10 175 ± 4 660 ± 5
N(r < Rt) 704 ± 26 845 ± 14 347 ± 8 70 ± 7 63 ± 3 690 ± 13
N(r < 30 pc) 1092 ± 17 1220 ± 14 770 ± 15 363 ± 20 317 ± 12 980 ± 9
Average mass loss [M/yr] ( ⋆ ⋆) 0.9 ± 0.1 0.8 ± 0.1 1.1 ± 0.1 1.3 ± 0.2 (=) 1.3 ± 0.2 0.9 ± 0.1

Notes. ( ⋆ )The mass loss in model M4 is more complex than in the other models, see the right panel of Fig. 15, thus the linear mass-loss average only serves as an orientation value. ( ⋆ ⋆)The average mass loss of each of the models has been calculated by a linear fit to the cluster mass loss over the simulation time (see Fig. 15, left panel). ( † )As described in Sect. 4, the M4 model is disrupted by a close encounter with a 107M lump. The disruption event occurs approximately 645 Myr after the start of the simulation, and we present the last column of values, which are averages of the values between 638 Myr and 643 Myr. This column shows the increase in velocity dispersion before the cluster is disrupted.

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