Models in order of increasing source accretion age and decreasing wind density.
|M ⋆||Ṁ acc||t acc||(1000 AU)||L hs||R sub|
|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.
Current usage metrics show cumulative count of Article Views (full-text article views including HTML views, PDF and ePub downloads, according to the available data) and Abstracts Views on Vision4Press platform.
Data correspond to usage on the plateform after 2015. The current usage metrics is available 48-96 hours after online publication and is updated daily on week days.
Initial download of the metrics may take a while.