Table 3
Global SFEs (SFEgl) and corresponding values of the SF duration (tSF) in N-body units (Eq. (12)) and in units of Myr for the adopted normalization parameters (using Eq. (18)).
| SFE gl | t SF | t SF |
|
|
| [NB] | [Myr] | [M⊙ pc-3] | [cm-3] | |
|
|
||||
| 0.05 | 2.14 | 0.39 | ||
|
|
||||
| 0.10 | 6.30 | 1.15 | 1490.73 | 26 405 |
| 0.13 | 9.58 | 1.75 | 1177.02 | 20 848 |
| 0.15 | 12.09 | 2.21 | 1037.99 | 18 386 |
| 0.20 | 19.53 | 3.56 | 813.52 | 14 410 |
| 0.25 | 28.74 | 5.25 | 680.92 | 12 061 |
|
|
||||
| 0.30 | 39.96 | 7.29 | 594.24 | 10 526 |
| 0.35 | 53.53 | 9.77 | 533.91 | 9457 |
| 0.40 | 69.94 | 12.77 | ||
| 0.45 | 89.85 | 16.40 | ||
| 0.50 | 114.22 | 20.85 | ||
Notes. The rows within the box highlight the non-isolated models selected for our simulations. We also show here the mean volume density of the clump (star + gas) inside the half-mass radius. Because we kept the stellar masses constant while varying the global SFE, we varied the fraction of unprocessed gas. When the global SFE increases, the mass of the residual gas decreases (keeping stellar mass constant), and as a consequence, the total volume density decreases as well.
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