Table 2
Canonical models of previous modeling work for HH 30 except W04.
| B96 | C01 | W02 | P06 | |
|
|
||||
| α | 2.2 | 2.367f | 2.25f | 2.2f |
| β | 1.45f | 1.289 | 1.25 | 1.25f |
| Rin [AU] | 0.5f | 0.07 | 0.03 | |
| Rout [AU] | ≳ 250f | 200f | 200f | 145 ± 20 |
| h100 [AU] | 15.5 | 15f | 17 | 15.5f |
| mdust [10-5 M⊙] | 6.0f | ≳ 0.67 | ≳ 1.5 | (2.7 ± 0.4) |
| L∗ [L⊙] | 1.0 | 0.2...0.9 | 0.2 (+0.04) | 0.2f |
| Teff [K] | 3000 | 3500f | 3700f (M1) | |
| i [°] | 82.5 | 84f | 84f | 81 ± 3 |
Notes. All parameters marked with the subscript f were fixed or taken from previous publications in the corresponding study. Numbers marked with ≳ are denoted as lower limits by the authors. W02 split luminosity into two contributions from the star and viscous dissipation. The dust masses assume a mass ratio of 1:100 between dust and gas.
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