Table 1
Stellar masses and wind parameters for the six selected stars of our sample of CSPNs for which FUSE observations are available.
| Object | M | Ṁ | v∞ |
| (M⊙) | (10-6M⊙/ yr) | (km s-1) | |
|
|
|||
| P04 parameter set | |||
|
|
|||
| NGC 2392 | 0.41 | 0.018 | 420a |
| IC 4593 | 1.11 | 0.062 | 850 |
| IC 418 | 1.33 | 0.072 | 800 |
| (Tc 1 | 1.37 | 0.021 | 900)b |
| NGC 6826 | 1.40 | 0.18 | 1200 |
| (He 2-131 | 1.39 | 0.35 | 450) |
|
|
|||
| K06c parameter set | |||
|
|
|||
| NGC 2392 | 0.86 | 0.471 | 400 |
| IC 4593 | 0.70 | 0.120 | 250 |
| IC 418 | 0.92 | 0.639 | 200 |
| (Tc 1 | 0.81 | 0.605 | 300) |
| NGC 6826 | 0.74 | 0.187 | 600 |
| (He 2-131 | 0.71 | 0.105 | 300) |
Notes. The upper part lists the parameters derived from the consistent UV analysis (P04), the lower part the parameters obtained from the optical analysis (K06), the mass-luminosity relation, and consistently calculated dynamics.
K97, P04, K06, and Kaschinski et al. (2012) deduced a terminal velocity of 400 km s-1 for this object from the UV spectrum. Herald & Bianchi (2011), who also note that the absorption extends to 300...400 km s-1, used 300 km s-1 for the terminal velocity, interpreting the gradual absorption seen in some profiles to be the result of shocked material moving at higher velocities.
No separate X-ray parameters were derived for the objects in parentheses, since their FUV spectra are very similar to that of IC 418 (see Fig. A.5) – it is therefore to be expected that the differences in the parameters are of minor importance for our present perspectives.
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