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arXiv 0812.1578astro-ph
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银河系行星状星云中的铁丰度

The Iron abundance in Galactic Planetary Nebulae

G. Delgado-Inglada, M. Rodriguez, A. Mampaso, K. Viironen

备注：
Accepted for publication in ApJ. 15 pages, 4 Postscript figures, corrected typos, Tables 2 and 3 corrected
发表信息：
Astrophys.J.694:1335-1348,2009; Erratum-ibid.729:77,2011
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摘要：

我们限制铁丰度的样品中的33个低电离银河系行星状星云（PNE）使用[Fe III]线和校正的贡献较高的电离状态与电离校正因子（ICF），考虑到原子数据的不确定性。我们在所有天体中发现了非常低的铁丰度，这表明它们90%以上的铁原子凝聚在尘埃颗粒上。这个数字是基于太阳铁的丰度，意味着尘埃与气体质量比的下限，仅由于铁，我们的样品的M_dust/M_gas>1.3x10^{-3}。不同PNe的损耗因子约为两个数量级，可能反映了其尘埃颗粒形成、生长或破坏的差异。然而，我们没有发现任何系统的差异计算的气态铁丰度为富C和富O PNE，这表明在这两种环境中类似的铁消耗效率。我们的样品PNe的铁丰度是类似的，得出以下相同的程序为一组10个银河系H II区域。这些高损耗因素表明，在分子云和AGB星中，难熔元素对尘埃颗粒的损耗效率很高，而在星际和星周电离气体中，尘埃的破坏效率很低。

英文摘要：

We constrain the iron abundance in a sample of 33 low-ionization Galactic planetary nebulae (PNe) using [Fe III] lines and correcting for the contribution of higher ionization states with ionization correction factors (ICFs) that take into account uncertainties in the atomic data. We find very low iron abundances in all the objects, suggesting that more than 90% of their iron atoms are condensed onto dust grains. This number is based on the solar iron abundance and implies a lower limit on the dust-to-gas mass ratio, due solely to iron, of M_dust/M_gas>1.3x10^{-3} for our sample. The depletion factors of different PNe cover about two orders of magnitude, probably reflecting differences in the formation, growth, or destruction of their dust grains. However, we do not find any systematic difference between the gaseous iron abundances calculated for C-rich and O-rich PNe, suggesting similar iron depletion efficiencies in both environments. The iron abundances of our sample PNe are similar to those derived following the same procedure for a group of 10 Galactic H II regions. These high depletion factors argue for high depletion efficiencies of refractory elements onto dust grains both in molecular clouds and AGB stars, and low dust destruction efficiencies both in interstellar and circumstellar ionized gas.

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