对星际水合氢离子（H3O+）的搜寻。

A search for interstellar H3O+.

作者信息

Wootten A, Boulanger F, Bogey M, Combes F, Encrenaz P J, Gerin M, Ziurys L

机构信息

National Radio Astronomy Observatory, Charlottesville, VA 22901, USA.

出版信息

Astron Astrophys. 1986;166:L15-8.

PMID:11542067

Abstract

The P (2,1) line of H3O+, the hydroxonium ion, a key species in ion-molecule chemistry, has been sought in the interstellar medium and in Halley's Comet. In OMC1 and SgrB2, a line was detected which may possibly be attributed to H3O+. Verification of this identification must be accomplished through observation of the P(3,2) line at 364 GHz, or detection of isotopic variants. If we were to assume that the detected line arises from H3O+, we can deduce a fractional abundance X(H3O+) in OMC1 and SgrB2 of approximately 10(-9) and a production rate in Comet Halley of Q(H3O+) 10(28)s-1. These results would place H3O+ among the more abundant molecular ions in the interstellar gas in agreement with theoretical predictions.

摘要

水合氢离子H₃O⁺的P(2,1)线是离子-分子化学中的关键物种，人们已在星际介质和哈雷彗星中寻找它。在猎户座分子云1（OMC1）和人马座B2（SgrB2）中，检测到了一条可能归因于H₃O⁺的谱线。必须通过观测364吉赫兹的P(3,2)线或检测同位素变体来完成对该鉴定的验证。如果我们假设检测到的谱线来自H₃O⁺，那么我们可以推断出OMC1和SgrB2中H₃O⁺的分数丰度X(H₃O⁺)约为10⁻⁹，哈雷彗星中H₃O⁺的产生率Q(H₃O⁺)为10²⁸s⁻¹。这些结果将使H₃O⁺跻身星际气体中较丰富的分子离子之列，这与理论预测相符。