Table 3
Models explored in this work in order of increasing source age.
| Model | Label | M* | Ṁacc | Ṁw |  |
 |
 / |
 /W0 |
|---|---|---|---|---|---|---|---|---|
| M⊙ | M⊙ yr−1 | M⊙ yr−1 | cm−3 | cm−3 | cm−3 | |||
| 0.1 | 5(−5) | 5(−6) | 1.3(11) | 5.5(10) | 2.4 | 5.9(13) | ||
| Class 0 | ⓐ | 0.1 | 2(−5) | 2(−6) | 5.0(10) | 2.2(10) | 2.3 | 2.3(13) |
| ⓑ | 0.1 | 1(−5) | 1(−6) | 2.5(10) | 1.1(10) | 2.3 | 1.1(13) | |
| 0.1 | 5(−6) | 5(−7) | 1.3(10) | 5.5(09) | 2.4 | 5.9(12) | ||
| Class I | ⓒ | 0.5 | 1(−6) | 1(−7) | 2.5(09) | 5.5(09) | 0.45 | 1.1(12) |
| Class II | 0.5 | 1(−7) | 1(−8) | 2.5(08) | 5.5(08) | 0.45 | 1.1(11) | |
Notes. Except for M* and Ṁw, all parameters have fixed values, namely R⋆ = 3 R⊙, Tvis = 4000 K, Vj = 100 km s−1, TK = 1000 K, Rin = 0.05 au, Rout = 0.3 au, R0 = 0.15 au, and z0 ∕R0 = 25. The accretion to ejection rate ratio is assumed to be 0.1 so that Ṁw = 0.1 Ṁacc for all models. Models in bold are studied in more details in Sect. 4.2 (see also Fig. 9) and are identified by a label. The last four columns are the density, the FUV radiation field, and the ratios
/
and
/W0
at the base of the computed streamline. Numbers in parentheses are powers of 10.
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