Table 7
Determined abundances for our best-fit DG Tau model.
| Molecule | DG Tau | Theoretical |
|
|
||
| Disk Fractional Abundances (w.r.t. H 2 )a | ||
| 12CO | 2.0 × 10-4 | 1.0 × 10-4 |
| 13CO | 3.3 × 10-6 | 1.7 × 10-6 |
| C18O | 4.0 × 10-7 | 2.0 × 10-7 |
| HCO+ | 2.0 × 10-11 | 1–100 × 10-11 |
| HCN | 5.0 × 10-12 | 1–100 × 10-11 |
| CN | 8.0 × 10-10 | 1–100 × 10-11 |
|
|
||
| Cloud Fractional Abundances (w.r.t. H 2 )b | ||
| 12CO | 2.0 × 10-4 | 8.0 × 10-5 |
| 13CO | 3.3 × 10-6 | – |
| C18O | 4.0 × 10-7 | – |
| HCO+ | 8.0 × 10-9 | 8.0 × 10-9 |
| HCN | 8.0 × 10-9 | 4–20 × 10-9 |
| CN c | – | 3–30 × 10-9 |
|
|
||
| Cloud Column Densities (cm -2 ) | ||
| 12CO | 6.0 × 1016 | ··· |
| 13CO | 1.0 × 1015 | ··· |
| C18O | 1.2 × 1014 | ··· |
| HCO+ | 2.4 × 1012 | ··· |
| HCN | 2.4 × 1012 | ··· |
| CN | – | ··· |
Notes.
The DG Tau abundances are constant throughout the disk (or disk-averaged), whereas the theoretical disk abundances from Aikawa et al. (2002) and van Zadelhoff et al. (2003) represent the ranges expected in the warm molecular layers only;
the theoretical cloud values are from Terzieva & Herbst (1998);
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