The main parameters of this grid are the stellar temperature T and the surface gravity ggrav. The spacing of the stellar temperatures is 1 kK, while it is 0.2 dex for the surface gravity. The luminosities are derived from the stellar evolution models published by Brott et al. (2011). The terminal wind velocity v is derived from the escape velocity, accounting for a metallicity scaling of (Z/Z)0.13 (Leitherer et al. 1992). The models are calculated for log [M/(M/yr)] values of -7.0. A clumping of D=10 is assumed. Wind clumping starts at the sonic point and increases outwards until a stellar radius of R = 10 R.
The abundances of C, N, O, Mg, Si, and Fe are obtained from Trundle et al. (2007). The abundances of the other elements are taken from the TMAP abundance list and subsequently scaled with a factor of 1/2 (corresponding to Zlmc/Z).
| Ion | No. of levels |
|---|---|
| H I | 22 |
| H II | 1 |
| He I | 35 |
| He II | 26 |
| He III | 1 |
| N I | 10 |
| N II | 38 |
| N III | 56 |
| N IV | 38 |
| N V | 20 |
| N VI | 14 |
| C I | 15 |
| C II | 32 |
| C III | 40 |
| C IV | 25 |
| C V | 29 |
| C VI | 1 |
| Ion | No. of levels |
|---|---|
| O I | 13 |
| O II | 37 |
| O III | 33 |
| O IV | 29 |
| O V | 36 |
| O VI | 16 |
| O VII | 15 |
| S III | 23 |
| S IV | 11 |
| S V | 10 |
| S VI | 1 |
| Mg I | 1 |
| Mg II | 32 |
| Mg III | 43 |
| Mg IV | 17 |
| Mg V | 20 |
| Si I | 20 |
| Ion | No. of levels |
|---|---|
| Si II | 20 |
| Si III | 24 |
| Si IV | 23 |
| Si V | 1 |
| P IV | 12 |
| P V | 11 |
| P VI | 1 |
| G I | 1 |
| G II | 3 |
| G III | 13 |
| G IV | 18 |
| G V | 22 |
| G VI | 29 |
| G VII | 19 |
| G VIII | 14 |
| G IX | 15 |
| G X | 1 |
Notes: Element "G" stands for the generic iron-group element, which combines the elements from Sc to Ni in solar relative mixture. In case of the "G" element, the number of levels given in the above table actually refers to superlevels.