CONSTRAINTS ON THE ABUNDANCES OF VARIOUS MOLECULES IN INTERSTELLAR ICE : LABORATORY STUDIES AND ASTROPHYSICAL IMPLICATIONS
CONSTRAINTS ON THE ABUNDANCES OF VARIOUS MOLECULES IN INTERSTELLAR ICE : LABORATORY STUDIES AND ASTROPHYSICAL IMPLICATIONS
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星际冰中各种分子丰度的限制：实验室研究和天体物理意义
DOI：
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发表时间：
1998
影响因子：
6.5
通讯作者：
J. Greenberg
中科院分区：
文献类型：
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作者：
N. Boudin;W. Schutte;J. Greenberg
乙烷、乙炔、乙醇、肼和过氧化氢要么根据理论模型预测在稠密云中颗粒的冰幔中丰富，要么被发现是由彗星产生的。我们对嵌入天体物理相关冰基质中的这些物种的光谱进行了测量。此外，我们还获得了氢离子（N2H + 5 ）的光谱，该离子可以通过无活化酸碱反应产生。将实验室结果与 NGC 7538:IRS 9 的 ISO 和地面光谱进行比较。与固体水相比，乙烷、乙醇和过氧化氢的严格上限分别为 < 0.4%、< 1.2% 和 <6.1%。这些结果为彗星和星际冰之间的关系以及颗粒表面反应的性质提供了一些重要信息。
Ethane, acetylene, ethanol, hydrazine and hydrogen peroxyde are either predicted by theoretical models to be abun- dant in the icy mantles on grains in dense clouds, or were found to be produced by comets. We present measurements of the spectra of these species embedded in astrophysically relevant ice matrices. Additionally, we obtained the spectrum of the hy- drozonium ion (N2H + 5 ) which could be produced by activation- less acid-base reactions. The laboratory results are compared to the ISO and ground{based spectra of NGC 7538:IRS 9. Strict upper-limits compared to the solid water could be found for ethane, ethanol and hydrogen peroxyde of < 0.4%, < 1.2%, and<6.1%, respectively. These results give some important in- formation on the relationship between cometary and interstellar ices and on the nature of grain surface reactions.