First detection of hydrogen isocyanide (HNC) in Titan's atmosphere
First detection of hydrogen isocyanide (HNC) in Titan's atmosphere
复制标题
首次在泰坦大气中检测到异氰化氢（HNC）
DOI：
10.1051/0004-6361/201118189
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发表时间：
2011
影响因子：
6.5
通讯作者：
A. González
中科院分区：
文献类型：
--
作者：
R. Moreno;E. Lellouch;L. Lara;R. Courtin;D. Bockelée;P. Hartogh;M. Rengel;N. Biver;M. Banaszkiewicz;A. González
我们报告的第一个识别的异氰化氢（HNC）在土卫六的大气中，从观察使用HIFI仪器的赫歇尔空间天文台。2010年6月14日和12月31日在土卫六上测量到一条543.897 GHz的HNC J = 6 → 5旋转跃迁的发射线。辐射传输模型表明，HNC的大部分位于400 km以上，柱密度范围为（0.6 - 1.5）× 10 13 cm-2，但观测结果无法确定其垂直分布。特别是HNC可能仅限于热层上部（1000公里），在这种情况下，其相对于HCN的局部丰度可能高达10.3。HNC可能主要在电离层水平（950-1150 km）由HCNH +和可能其他较重的腈离子的解离重组形成。HNC的电离层损失发生质子化与XH +离子。在中性气氛中的其他形成（例如从N（4 S）+3 CH 2）和损失途径（例如从异构化到HCN）仍有待研究。
We report on the first identification of hydrogen isocyanide (HNC) in Titan's atmosphere, from observations using the HIFI instrument on the HerschelSpace Observatory. An emission line from the HNC J = 6 → 5 rotational transition at 543.897 GHz was measured in Titan on June 14 and December 31, 2010. Radiative transfer modeling indicates that the bulk of HNC is located above 400 km, with a column density in the range (0.6−1.5) × 10 13 cm −2 , but the observations cannot establish its vertical profile. In particular HNC could be restricted to the upper thermosphere (∼1000 km), in which case its local abundance relative to HCN could be as high as ∼0.3. HNC is probably formed mostly at ionospheric levels (950-1150 km) from dissociative recombination of HCNH + and possibly other heavier nitrile ions. Ionospheric loss of HNC occurs by protonation with XH + ions. Additional formation (e.g. from N( 4 S) + 3 CH2) and loss routes (e.g. from isomerization to HCN) in the neutral atmosphere remain to be investigated.
影响因子：
2.8
作者：
Galand, Marina;Yelle, Roger;Coates, Andrew
通讯作者：
Coates, Andrew