Table 1.
Values of the integrated deficit, 𝒟, for runs of models with turbulence.
| Model | vturb km s−1 | Ṁ M⊙ Myr−1 | v0 | 𝒟 | Note |
|---|---|---|---|---|---|
| 1 | 0 | 0.002 | 0 | 0.61 | |
| 2 | 1 | 0.002 | 0 | 0.61 | |
| 3 | 1 | 0.002 | 0 | 0.60 | coulomb |
| 4 | 1 | 0.002 | 0 | 0.47 | + photo-el. |
| 5 | 2 | 0.002 | 0 | 0.64 | |
| 6 | 1 | 0.004 | 0 | 0.55 | |
| 7 | 1 | 0.010 | 0 | 0.41 | |
| 8 | 1 | 0.002 | vff | 0.54 | |
| 9 | 1 | 0.002 | 0 | 0.60 | r0 = 1000 AU |
| 10 | 1 | 0.002 | 0 | 0.58 | δρ |
| 11 | 1 | 0.002 | 0 | 0.60 | ρ−2, r0 = 1000 AU |
| 12 | 1 | 0.002 | 0 | 0.60 | Closed box |
| 13 | 1 | 0.002 | 0 | 0.61 | Semi-closed box |
Notes. The parameters of the models are the 1D turbulence parameter vturb in km s−1, and the gas-flow rate Ṁ in M⊙ Myr−1. The initial condition for the dust grains at distance r0 = 10 000 AU from the star is v0 = 0 except for a model where v0 is set to the free-fall velocity vff of the gas at r0. All models were run neglecting the coulomb forces, except two, marked “coulomb” and “+ photo-el”. For these, the coulomb forces, without and with the photoelectric charging of the dust grains, respectively, were included schematically (see text). The model marked δρ in the last column was run with fluctuating density, see text, and the following model with a ρ ∝ r −2 dependence and r0 = 1000 AU. The two last lines represent runs where the star was enclosed in a 0.125 pc3 cubic box with six reflecting walls, to simulate the contributions of new grains from surrounding stars, and five reflecting walls, respectively.
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