Table 1
Characteristic masses from various numerical streaming instability studies.
| Reference | Z | γ | Π | τs | Fitting type | Characteristic mass [ ] |
|||
|---|---|---|---|---|---|---|---|---|---|
| Johansen et al. (2015) | 0.02 | 0.1 | 0.05 | 0.3 | STPL | 9.1 × 10−5 | |||
| Simon et al. (2016) | 0.02 | 0.1 | 0.05 | 0.3 | SPL | 4.5 × 10−4 (a) | |||
| 0.02 | 0.05 | 0.05 | 0.3 | SPL | 2.4 × 10−4 | ||||
| 0.02 | 0.02 | 0.05 | 0.3 | SPL | 2.0 × 10−4 | ||||
| Schäfer et al. (2017) | 0.02 | 1∕π | 0.05 | 0.314 | VTPL | Their Table 2 (b) | |||
| Abod et al. (2019) | 0.1 | 0.02 | 0-0.1 | 0.05 | STPL | Their Table 1 (c) | |||
| Li et al. (2019) | 0.1 | 0.05 | 0.05 | 2.0 | STPL, VTPL, BPL | 4.1 × 10−5, 6.3 × 10−7, 1.6 × 10−6 | |||
| 0.02 | 0.05 | 0.05 | 0.3 | STPL, VTPL, BPL | 2.7 × 10−5, 8.1 × 10−6, 3.8 × 10−6 | ||||
Notes. The characteristic mass Mpl is adopted to be Mexp from the STPL and VTPL fittings, or to be Mbr from the BPL fitting (see Eq. (23) of Li et al. 2019). For the SPL fitting, we adopt the largest planetesimal mass as an upper limit of Mpl. All these masses are provided in the code unit (
). The data are adopted from Johansen et al. (2015), Simon et al. (2016), Schäfer et al. (2017), Abod et al. (2019), and Li et al. (2019). (a) The mass of the largest planetesimal(the upper limit of Mpl) (b) There are six simulations with different numerical resolutions and box sizes. (c) There are ten simulations with different Π and different times when the particles’ self-gravity is initiated.
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