Table 1
Syllabus of the different simulations, with the thermal-to-gravitational energy ratios α, and the maximum grain sizes Smax.
| Model | α | Smax (cm) | μ | ϕmag (°) | Ambipolar | tcore (kyr) | St0,10 |
|---|---|---|---|---|---|---|---|
| MMMRN | 0.5 | 0.1 | – | – | – | 72.84 | 1.22 × 10−2 |
| MRN | 0.5 | 2.5 × 10−5 | – | – | – | 73.6 | 1.06 × 10−5 |
| 100MICMRN | 0.5 | 0.01 | – | – | – | 72.9 | 1.72 × 10−3 |
| MMMRNA0.25 | 0.25 | 0.1 | – | – | – | 23 | 4.31 × 10−3 |
| MMMRNMHD | 0.5 | 0.1 | 5 | 40 | NO | 81.1 | 1.22 × 10−2 |
| MMMRNNIMHD | 0.5 | 0.1 | 5 | 40 | YES | 81.1 | 1.22 × 10−2 |
| Initial cloud mass | Number of dust bins | ||||||
| 1 M⊙ | 10 | ||||||
Notes. The initial mass-to-flux ratio μ as well as the tilt between the magnetic field and the rotation axis ϕmag are given for simulations with magnetic field. Additionally, we provide the formation time of the FHSC tcore, the initial Stokes number of the largest grains St0,10, the mass of the initial core, and the number of dust bins.
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