The evolution of planetary nebulae - VI. On the chemical composition of the metal-poor PN G135.9+55.9

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Table 4:

Summary of our best-match model parameters.
Parameter	PN G135.9+55.9	$Z\ensuremath{_{{\rm GD}}}$
Spectrum	black body
Stellar mass, M	0.595 $\ensuremath{{M}_{\odot}}$
Model age, t	8982 yr
Stellar effective temperature, $\ensuremath {T_{\rm eff}}$	138 049 K
Stellar luminosity, L	$2994~\ensuremath{{L}_{\odot}}$
Central star wind, $L_{\rm wind}=0.5\dot{M}v^2_\infty$	$\dot{M}\propto Z^{0.69}$ , $v_\infty\propto Z^{0.13}$
AGB wind	$\rho\propto r^{-3.25}$ , $v = 10~\ensuremath{{\rm km}~{\rm s}^{-1}}$ ,
	$n_{r=3\times10^{16}~{\rm cm}} = 1$ $\times$ $10^5~\ensuremath{{\rm cm}^{-3}}$
Abundances, $\epsilon_i = \log~(n_i/n_{\rm H})+12$ :
He	10.88	11.04
C	$\ensuremath{\phantom{0}}$ 7.90	$\ensuremath{\phantom{0}}$ 8.89
N	$\ensuremath{\phantom{0}}$ 7.47:	$\ensuremath{\phantom{0}}$ 8.39
O	$\ensuremath{\phantom{0}}$ 6.74	$\ensuremath{\phantom{0}}$ 8.65
Ne	$\ensuremath{\phantom{0}}$ 6.96	$\ensuremath{\phantom{0}}$ 8.01
S	[5.94]	$\ensuremath{\phantom{0}}$ 7.04
Cl	[4.22]	$\ensuremath{\phantom{0}}$ 5.32
Ar	[5.36]	$\ensuremath{\phantom{0}}$ 6.46
Distance, d	18 kpc
Visual magnitude, $m_{\rm V}$	19.5 mag
Nebular density, $\langle\ensuremath{n_{\rm e}}\rangle$	65 $\ensuremath{{\rm cm}^{-3}}$
Nebular temperature, $\langle\ensuremath{T_{\rm e}}\rangle$	21 100 K
Nebular $\ensuremath{{\rm H}\beta}$ -luminosity, $L(\ensuremath{{\rm H}\beta} )$	0.193 $\ensuremath{{L}_{\odot}}$
Model HWHM velocity, $V_{\rm HWHM}$	$41.8~\ensuremath{{\rm km}~{\rm s}^{-1}}$

Notes. The element abundances $\epsilon_{i}$ are used as input in the calculation of our radiation hydrodynamic models; the values of S, Cl, and Ar are not fitted, but only scaled. $Z\ensuremath{_{{\rm GD}}}$ denotes the mean abundance distribution in the Galactic disk (cf. Sect. 4.1).

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