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Table 2
Summary of models from Fig. 3.
| Panel | Model | Density | Abundance | Luminosity | |
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| a) | A1 | ρ ∝ r-1.5 | X0 (constant) | 1.1 L⊙ | |
| A2 | ρ ∝ r-1.5 | X0/ 8 (constant) | 1.1 L⊙ | ||
| A3 | ρ ∝ r-1.5 | 8 X0 (constant) | 1.1 L⊙ | ||
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| b) | B1 | ρ ∝ r-1.5 | X0 for r<r20 K | X0/ 100 for r>r20 K | 1.1 L⊙ |
| B2 | ρ ∝ r-1.5 | X0 for r<r20 K | X0/ 10 for r>r20 K | 1.1 L⊙ | |
| B3 | ρ ∝ r-1.5 | 10 X0 for r<r20 K | X0/ 10 for r>r20 K | 1.1 L⊙ | |
| B4 | ρ ∝ r-1.5 | X0 for r<r20 K – and gradual decrease from X0 at rout to X0/ 100 at r20 K | 1.1 L⊙ | ||
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| c) | C1 | ρ ∝ r-1.5 | X0 for r<r20 K | X0/ 10 for r>r20 K | 5 L⊙ |
| C2 | ρ ∝ r-1.5 | X0 for r<r30 K | X0/ 10 for r>r30 K | 30 L⊙ | |
| C3 | ρ ∝ r-2.0 | X0 for r<r30 K | X0/ 10 for r>r30 K | 50 L⊙ | |
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| d) | D1 | ρ ∝ r-1.5 | X0 for r<r20 K | X0/ 100 for r>r20 K | 1.1 L⊙ |
| D2 | ρ ∝ r-1.5 | X0 for r<r20 K | X0/ 100 for r>r20 K | 1.1 L⊙; ISRF × 5a | |
| D3 | ρ ∝ r-1.5 | X0 for r<r20 K | X0/ 100 for r>r20 K | 1.1 L⊙; ISRF × 50a | |
Notes.X0 is a C18O abundance of 2 × 10-7 with respect to H2, corresponding to a canonical CO abundance of 10-4.
(a)
Interstellar radiation field (ISRF) enhanced by a factor of 5 and 50 above the standard ISRF described by Black (1994).
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