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Detection of CH+, CH and H2 Molecules in the Young Planetary Nebula IC 4997
Publications of the Astronomical Society of the Pacific ( IF 3.3 ) Pub Date : 2020-06-09 , DOI: 10.1088/1538-3873/ab9097
N. Kameswara Rao 1, 2 , David L. Lambert 3 , Arumalla B. S. Reddy 1 , D. A. Garca-Hernndez 4, 5 , Arturo Manchado 4, 5, 6 , J. J. Daz-Luis 4, 5
Affiliation  

We have detected CH$^{+}$ and CH molecular absorption lines from the young compact planetary nebula IC 4997 from high resolution optical spectra. A high-resolution infra-red (H and K bands) spectrum provides detection of H$_2$ emission lines amongst many other lines. The H$_2$ lines provide an excitation temperature of 2100 K which may result from UV fluorescence in the envelope or from shocks formed at the interface between an expanding outflow of ionized gas and the neutral envelope ejected when the star was on the AGB. It is suggested that the CH$^+$ may result from the endothermic reaction C + H$_2$ $\rightarrow$ CH$^+$ + H. Intriguingly, CH$^{+}$ and also CH show a higher expansion velocity than H$_{\rm 2}$ emission suggesting they may be part of the post-shocked gas.

中文翻译:

检测年轻行星状星云中的 CH+、CH 和 H2 分子 IC 4997

我们已从高分辨率光谱中检测到年轻致密行星状星云 IC 4997 的 CH$^{+}$ 和 CH 分子吸收线。高分辨率红外(H 和 K 波段)光谱可检测许多其他线中的 H$_2$ 发射线。H$_2$ 线提供了 2100 K 的激发温度,这可能是由于包层中的紫外线荧光或由于在恒星位于 AGB 上时在膨胀的电离气体流出和喷射出的中性包层之间的界面处形成的冲击造成的。表明 CH$^+$ 可能来自吸热反应 C + H$_2$ $\rightarrow$ CH$^+$ + H。有趣的是,CH$^{+}$ 和 CH 显示出更高的膨胀速度比 H$_{\rm 2}$ 排放表明它们可能是震后气体的一部分。
更新日期:2020-06-09
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