Table 2
Chemical reactions affecting the H2O gas-phase abundance in our models.
| Reaction | Adopted rate per unit volume (cm-3s-1) | Refs. |
|
|
||
| O + H2→ OH + H |
|
1 |
| OH + H2→ H2O + H |
|
1 |
| H3O+ + e−→ OH + H2 |
|
2 |
| H3O+ + e−→ H2O + H |
|
2 |
| H2O + FUV → OH + H | 8 × 10-10χexp(−1.7AV) n(H2O) | 3 |
| H2O + FUV → H2O+ + e− | 3.3 × 10-11χexp(−3.9AV) n(H2O) | 3 |
Notes. n(X) is the number density of species X in cm-3, χ is the unattenuated incident stellar FUV field in units of the Draine interstellar FUV field (see Sect. 2.4.4 of Panoglou et al. 2012), AV is the visual extinction between the star and the local point provided by inner dusty wind streamlines (see Eq. (17) of Panoglou et al. 2012).
Reference. (1) Cohen & Westberg (1983); (2) Millar et al. (1989); (3) van Dishoeck (1988).
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