Table 1.
Estimations with n0 = 100 cm−3, B1, and B2 are the mean magnetic field strength using k = 1/2 and k = 1/3, respectively, assuming an additional flux loss αad = 10−2 due to ambipolar diffusion.
| M* | R* |  |
B1 | B2 | Beq |
|---|---|---|---|---|---|
| (M⊙) | (R⊙) | (kg m−3) | (G) | (G) | (G) |
| 1 | 13 | 0.64 | 166.34 | 7.72 | 341 |
| 1 | 6 | 6.53 | 780.85 | 36.24 | 955 |
| 1 | 3 | 52.23 | 3.1 × 103 | 144.98 | 2.4 × 103 |
| 1 | 2 | 176.27 | 7 × 103 | 326.20 | 4.1 × 103 |
| 1 | 1.8 | 241.80 | 8.7 × 103 | 402.71 | 4.8 × 103 |
| 3 | 22 | 0.40 | 120.81 | 5.61 | 1.5 × 103 |
| 3 | 15 | 1.25 | 259.88 | 12.06 | 2.5 × 103 |
| 3 | 13 | 1.93 | 345.99 | 16.06 | 3.1 × 103 |
| 3 | 11 | 3.18 | 483.24 | 22.43 | 3.8 × 103 |
| 3 | 9 | 5.80 | 721.88 | 33.51 | 5 × 103 |
| 5 | 45 | 0.08 | 40.59 | 1.88 | 1.6 × 103 |
| 5 | 30.5 | 0.25 | 88.36 | 4.10 | 2.7 × 103 |
| 5 | 21.6 | 0.70 | 176.17 | 8.18 | 4.3 × 103 |
| 5 | 19.3 | 0.98 | 220.67 | 10.24 | 5 × 103 |
| 5 | 18 | 1.21 | 253.69 | 11.78 | 5.5 × 103 |
Notes. Beq denotes that equipartition field strength within the protostar that is required to suppress convection. Here, the recoupling between the density and the magnetic field is assumed to happen at a number density of 1015 cm−3, and subsequently to follow a spherically symmetric contraction. For the purpose of comparison, we adopt here the fully convective protostellar models employed by Moss (2003).
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