Table 8
Physical parameters estimated with the model for the studied prolyds.
| Object | P trans | Gas temperature at | N env | r disk | Ṁ supercritical | Ṁ subcritical | Ṁ observed |
| the disk surface (K) | (cm-2) | (AU) | (M⊙/yr) | (M⊙/yr) | (M⊙/yr) | ||
|
|
|||||||
| 105-600 | 1.00 | 1100 | 1.4e+21 | 2500a | 7.5e-05 | ... | 1e-06 |
| HST10 | 1.05 | 1150 | 2.0e+21 | 85b | 5.0e-07 | 1.7e-08 | (7 ± 5)e-07 |
| 244-440 | 1.01 | 1270 | 1.9e+21 | 193b | 1.4e-06 | 8.2e-09 | (15 ± 7)e-07 |
| 203-506 | 1.12 | 1080 | 1.0e+21 | 150b | 9.4e-08 | 9.9e-09 | ... |
Notes. Densities and temperature are derived form the best fit model for each object. The observed mass-loss rates derived at the ionisation front are from Henney & O’Dell (1999) for HST10 and 244-440, and derived by us from Hα images for 105-600 (see text for details). A central star of 1 M⊙ is used in the calculation of the mass-loss rate for 105-600 while, for the Orion proplyds, we used a 0.1 and 1 M⊙ for the supercritical and subcritical cases respectively.
Disk radius roughly approximated by this study (see Sect. 4.1.2).
Disk radius estimated by spatially resolved observation: HST10 from Chen et al. (1998), 244-440 and 203-506 from Vicente & Alves (2005).
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