ISO Spectra of Planetary Nebulae
ISO Spectra of Planetary Nebulae
复制标题
行星状星云的 ISO 光谱
DOI：
10.1017/s0074180900208826
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发表时间：
2003
期刊：
影响因子：
--
通讯作者：
S. Kwok
中科院分区：
文献类型：
--
作者：
K. Volk;S. Kwok
众所周知，自红外天文卫星使命以来，尘埃排放占PNe能量输出的很大一部分（Zhang & Kwok 1991）。虽然PNE中的尘埃成分一直被认为是AGB星的残余物（Kwok 1982），但我们现在知道PNE中的尘埃具有更丰富的化学成分。除了在AGB星中常见的无定形硅酸盐和SiC特征外，还发现PNe具有强烈的芳香族红外特征（Russell et al. 1977）、结晶硅酸盐特征（沃茨et al. 1997）和30 μm处的不明发射特征（Forrest et al. 1981）。在本文中，我们显示了ISO光谱的一些PNe说明不同的尘埃化学PNe。
It has been well known since the IRAS mission that dust emission represents a significant fraction of the energy output from PNe (Zhang & Kwok 1991). Although the dust component in PNe was long thought to be due to the remnants of the envelopes of AGB stars (Kwok 1982), we now know that dust in PNe has a much richer chemical composition. In addition to amorphous silicates and SiC features commonly seen in AGB stars, PNe have been found to have strong aromatic infrared features (Russell et al. 1977), crystalline silicate features (Waters et al. 1997), and an unidentified emission feature at 30 μm (Forrest et al. 1981). In this paper, we show the ISO spectra of a number of PNe illustrating the diverse dust chemistry in PNe.