Table 1
Stellar parameters and results of the SED and CO line-emission models.
| Source | T∗ | L∗ | Ri | Ti | D | τ d | υ ∞ | β | d/g | Ṁ | R e | δ |
|
| [K] | [L⊙] | [1013 cm] | [K] | [pc] | [km/s] | [10-2] | [10-7 M⊙] | [1016 cm] | |||||
|
|
|||||||||||||
| R Dor | 2400 | 6500 | 6.6 | 1680 | 59 | 0.05 | 5.7 | 1.5 | 0.08 | 1.6 | 1.6 | 1.0 | 0.65 |
| R Cas | 1800 | 8725 | 25 | 1050 | 172 | 0.09 | 10.5 | 2.5 | 0.04 | 8.0 | 3.2 | 0.9 | 1.7 |
| TX Cam | 2400 | 8600 | 30 | 845 | 380 | 0.4 | 17.5 | 1.5 | 2.6 | 40 | 6.6 | 0.9 | 3.1 |
| IK Tau | 2100 | 7700 | 18 | 960 | 265 | 1.0 | 17.5 | 1.5 | 0.5 | 50 | 7.5 | 0.9 | 2.9 |
Notes. T∗ and L∗ are the stellar effective temperature and luminosity, respectively. Ri is the inner radius from which the CSE is modelled, and Ti the temperature at the inner radius. D is the distance to the source. τd is the dust optical depth at 10 μm, υ∞ the terminal gas expansion velocity, β the exponent of the velocity law, d/g the derived dust-to-gas ratio, Ṁ the gas mass-loss rate, Re the CO-photodissociation radius, δ the average ratio between integrated model and observed line intensities, and the reduced χ2 value of the best-fit model.
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