Table A.1
Minimum clumping structure and Ṁmax of HD 198474 derived in this work for the interval of stellar parameters provided by Markova & Puls (2008) (see text and Figure A.2).
| Teff | log g | υ∞ | β | YHe | R* | Ṁmax |  |
 |
 |
 |
 |
log Q′ | Sol. |
|---|---|---|---|---|---|---|---|---|---|---|---|---|---|
| 17.5 | 2.12 | 470 | 1.3 | 0.2 | 35.8 | ≤ 0.38 | 40.0 | 6.5 | 1.0 | 10.0 | 1.0 | -8.75 | 1a |
| 0.1 | ≤ 0.322 | 40.0 | 6.5 | 1.0 | 10.0 | 1.0 | -8.83 | 1b | |||||
| 200 | 1.3 | 0.2 | ≤ 0.165 | 45.0 | 6.0 | 1.0 | 10.0 | 1.0 | -9.11 | 2a | |||
| 0.1 | ≤ 0.14 | 45.0 | 6.0 | 1.0 | 10.0 | 1.0 | -9.18 | 2b |
Notes. Teff is in kK; log g is the gravity without centrifugal correction; YHe denotes thehelium fraction by number used in the simulations; and υ∞, R* and Ṁmax are in units of km s−1, R⊙ and 10−6 M⊙ yr−1, respectively.
gives the maximum possible clumping factor in Region 4 still consistent with the data. log Q′ = log (Ṁmax/R*1.5) is in units of M⊙ yr−1 and R⊙, and, for clarity, the last column indicates the label for the solution displayed in Figures A.2 and A.6.
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