Table 1
Models in order of increasing source accretion age and decreasing wind density.
| M ⋆ | Ṁ acc | t acc |  (1000 AU) |
L hs | R sub |
| (M⊙) | (M⊙ yr-1) | (yr) | (cm-3) | (L⊙) | (AU) |
|
|
|||||
| model X0 = Extreme Class 0 | |||||
| 0.1 | 2 × 10-5 | 5 × 103 | 2.3 × 106 | 10.5 | 0.63 |
|
|
|||||
| model S0 = Standard Class 0 (reference model) | |||||
| 0.1 | 5 × 10-6 | 2 × 104 | 6 × 105 | 2.6 | 0.31 |
|
|
|||||
| model X1 = Extreme Class 1 | |||||
| 0.5 | 5 × 10-6 | 105 | 2.5 × 105 | 13.1 | 0.64 |
|
|
|||||
| model S1= Standard Class 1 | |||||
| 0.5 | 10-6 | 5 × 105 | 5 × 104 | 2.6 | 0.27 |
Notes. M⋆ is the stellar mass, Ṁacc the accretion rate through the disk, and tacc ≡M⋆/Ṁacc the characteristic accretion age. (1000 AU) is the H2 density at 1000 AU of an envelope in free fall at rate Ṁacc onto a star of mass M⋆. It scales as ṀaccM⋆-0.5, like the wind density field, and thus acts as a proxy for the latter quantity. Lhs ≡ 0.5GM⋆Ṁacc/R⋆ is the accretion hot-spot luminosity and Rsub the dust sublimation radius as calculated by DUSTY (see Appendix C). For each source model, synthetic line profiles were calculated for a grid of maximum launch radii 
= 3.2, 6.4, 12.8, and 25.6 au and inclination angles i = 30°, 60°, and 80° from pole-on.
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