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Astron. Astrophys. 342, 233-256 (1999)

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Appendix A: chemical reactions used in the modelling

A.1. Cosmic ray ionisation (units s-1 mol[FORMULA]

[EQUATION]

[EQUATION]

A.2. Ion-molecule reactions (units cm3 s-1 mol[FORMULA]

[EQUATION]

[EQUATION]

[EQUATION]

[EQUATION]

[EQUATION]

[EQUATION]

A.3. Neutral-neutral reactions (units cm3 s-1 mol[FORMULA]

[EQUATION]

[EQUATION]

A.4. Electron recombination (units cm3 s-1 mol[FORMULA]

[EQUATION]

[EQUATION]

[EQUATION]

[EQUATION]

[EQUATION]

A.5. Photoreactions (units s-1 mol[FORMULA]

[EQUATION]

[EQUATION]

[EQUATION]

where [FORMULA] is the CO self-shielding factor

[EQUATION]

[EQUATION]

[EQUATION]

A.6. Charge transfer reactions (unit cm3 s-1 mol[FORMULA]

[EQUATION]

Appendix B: conservation conditions

Along with the above sets of reactions, we also use the following conservation conditions when evolving the chemistry

[EQUATION]

[EQUATION]

[EQUATION]

The following fractional abundances are assumed for our models:

[EQUATION]

[EQUATION]

[EQUATION]

[EQUATION]

Appendix C: initial conditions

When evolving the time-dependent chemistry, we use the following initial conditions:

[EQUATION]

[EQUATION]

[EQUATION]

[EQUATION]

[EQUATION]

[EQUATION]

[EQUATION]

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© European Southern Observatory (ESO) 1999

Online publication: December 22, 1998
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