Table A.1
Parameters used in the PDR code as input in the .in files.
| Parameter | Description | Value |
|
|
||
| modele | Basename for the output files | see Appendix A |
| chimie | Chemistry file | chimie08 a |
| ifafm | Number of global iterations | 20 |
| Avmax | Integration limit in AV | see Appendix A |
| densh | Initial density (cm-3) | see Appendix A |
| F_ISRF | ISRF expression flag | 1 b |
| radm | ISRF scaling factor χm | see Appendix A |
| radp | ISRF scaling factor χp | see Appendix A |
| srcpp | Additional radiation field source | none.txt |
| d_sour | Star distance (pc) | 0 c |
| fmrc | Cosmic rays ionisation rate (10-17 s-1) | 5 |
| ieqth | Thermal balance computation flag | 1 d |
| tgaz | Initial temperature (K) | see Appendix A |
| ifisob | State equation flag | see Appendix A |
| fprofil | Density-Temperature profile file | see Appendix A |
| presse | Initial pressure (K cm-3) | see Appendix A |
| vturb | Turbulent velocity (km s-1) | see Appendix A |
| itrfer | UV transfer method flag | 0 e |
| jfgkh2 | Minimum J level for FGK approximation | 0 |
| ichh2 | H + H2 collision rate model flag | 2 f |
| los_ext | Line of sight extinction curve | Galaxy g |
| rrr | Reddening coefficient RV = AV/EB − V | 3.1 h |
| cdunit | Gas-to-dust ratio CD = NH/EB − V (cm-2) | 5.8 × 1021 g |
| alb | Dust albedo | 0.42 g |
| gg | Diffusion anisotropy factor ⟨cosθ⟩ | 0.6 g |
| gratio | Mass ratio of grains/gas | 0.01 g |
| rhogr | Grains mass density (g cm-3) | 2.59 i |
| alpgr | Grains distribution index | 3.5 g |
| rgrmin | Grains minimum radius (cm) | 3 × 10-7 g |
| rgrmax | Grains maximum radius (cm) | 3 × 10-5 g |
| F_DUSTEM | DUSTEM activation flag | 0 j |
| iforh2 | H2 formation on grains model flag | 0 k |
| istic | H sticking on grain model flag | 4 l |
Notes.
Uses expressions based on Mathis et al. (1983) and Black (1994) rather than Draine (1978).
Thermal balance is computed for each point in the cloud, using the temperatures given by the .pfl file as initial guesses.
Use the Federman et al. (1979, FGK) approximation for the H2 lines in the UV.
Use the values compiled by Le Bourlot et al. (1999) with reactive collisions from Schofield (1967).
See Table 4 of Le Petit et al. (2006), which quotes values from Fitzpatrick & Massa (1990) for the extinction curve, Bohlin (1978); Rachford et al. (2002) for CD, Mathis (1996) for the dust albedo, Weingartner & Draine (2001) for ⟨cosθ⟩, Mathis et al. (1977) for the grain size distribution parameters.
See for instance Cardelli et al. (1989).
Taken from Gonzalez Garcia et al. (2008).
Do not couple to the DUSTEM code (Compiègne et al. 2011).
Energy released by H2 formation on dust grains is equally split between grain excitation, H2 kinetic energy and internal energy. See Sect. 6.1.2 in Le Petit et al. (2006) for details.
See Appendix E5 in Le Petit et al. (2006).
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