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).
Current usage metrics show cumulative count of Article Views (full-text article views including HTML views, PDF and ePub downloads, according to the available data) and Abstracts Views on Vision4Press platform.
Data correspond to usage on the plateform after 2015. The current usage metrics is available 48-96 hours after online publication and is updated daily on week days.
Initial download of the metrics may take a while.