Table 2
Stellar and wind parameters of the models used to compute the synthetic spectra presented in this work for the two CSPNs NGC 6826 and NGC 2392.
| Teff | R | log L | M | log g | Ṁ | v∞ | Parameter source | Matches | |||
| (K) | (R⊙) | (L⊙) | (M⊙) | (cm/s2) | (10-6 M⊙/yr) | (km s-1) | stellar | wind | consistent? | observation? | |
|
|
|||||||||||
| NGC 6826 | |||||||||||
| 50 000 | 2.0 | 4.4 | 0.92 | 3.8 | 0.26 | 1200 | K97 | K97 | no | yes | |
| ′′ | ′′ | ′′ | ′′ | ′′ | 0.50 | 850 | ′′ | this work | yes | no | |
| 46 000 | 1.8 | 4.11 | 0.74 | 3.8 | 0.08 | 1200 | K06 | K06 | no | – | |
| 44 000 | 2.2 | 4.2 | 1.40 | 3.9 | 0.18 | 1200 | P04 | P04 | yes | yes | |
| ′′ | ′′ | ′′ | 0.88 | 3.7 | 0.25 | 360 | this work | this work | yes | no | |
|
|
|||||||||||
| NGC 2392 | |||||||||||
| 45 000 | 2.5 | 4.4 | 0.91 | 3.6 | ≤0.03 | 400 | K97 | K97 | no | yes | |
| ′′ | ′′ | ′′ | ′′ | ′′ | 0. 32 | 400 | ′′ | this work | yes | no | |
| 44 000 | 2.4 | 4.30 | 0.86 | 3.6 | ≤0. 05 | 400 | K06 | K06 | no | – | |
| 40 000 | 1.5 | 3.7 | 0.41 | 3.7 | 0.018 | 420 | P04 | P04 | yes | yes | |
|
|
|||||||||||
Notes. P04 refers to the parameters derived by Pauldrach et al. (2004) from an analysis of the UV spectra, K97 refers to the optical analysis of Kudritzki et al. (1997), and K06 refers to the optical analysis of Kudritzki et al. (2006) (a dash in the “matches observation?” column indicates that a comparison to observations was not shown in the paper). “Consistent” means that the wind parameters are consistent with the stellar parameters as determined by our hydrodynamic calculations of the radiative driving force. We note that Kudritzki et al. (2006) obtained a much lower mass loss rate for NGC 6826 than Kudritzki et al. (1997).
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