Table 1: Objects selected for comparison with our hydrodynamical models. The effective temperatures of the central stars are from Méndez et al. (1992), and the spectroscopic expansion velocities from the decomposition of [O III] line profiles (Paper II, Table 4 therein).
Object $T_{\rm eff}$ $V_{\rm rim}$ $V_{\rm shell}$

[K] [km s^-1] [km s^-1]

NGC 6826 50 000 8.0 27.0

IC 2448 65 000 17.5 33.3

NGC 3242 75 000 19.5 35.7

**Table 1:** Objects selected for comparison with our hydrodynamical models. The effective temperatures of the central stars are from Méndez et al. (1992), and the spectroscopic expansion velocities from the decomposition of [O III] line profiles (Paper II, Table 4 therein).
Object	$T_{\rm eff}$	$V_{\rm rim}$	$V_{\rm shell}$
	[K]	[km s^-1]	[km s^-1]
NGC 6826	50 000	8.0	27.0
IC 2448	65 000	17.5	33.3
NGC 3242	75 000	19.5	35.7

Source LaTeX | All tables | In the text

	1 Introduction
	2 The hydrodynamical model
	3 The models in comparison with observations
	4 The expansion parallaxes
	5 Summary and discussion
	References
	Online Material
	Appendix A:Hydrodynamical PNe sequence with a 0.696 M $_{\odot }$ central-star