基于CN自由基的火星再入流场温度测量

林鑫; 余西龙; 李飞; 张少华; 辛建国; 张新宇

doi:10.6052/0459-1879-13-224

基于CN自由基的火星再入流场温度测量

doi: 10.6052/0459-1879-13-224

1 中国科学院力学研究所高温气体动力学国家重点实验室, 北京 100190
2 北京理工大学光电学院, 北京 100081

基金项目: 国家自然科学基金资助项目（11002148，91216101）.

详细信息

作者简介:
余西龙，研究员，主要研究方向：高焓非平衡流动、激光光谱诊断.E-mail：xlyu@imech.ac.cn

中图分类号: V556.4
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出版历程
- 收稿日期: 2013-07-08
- 修回日期: 2013-09-12
- 刊出日期: 2014-03-18

TEMPERATURE MEASUREMENTS IN SIMULATED MARS ATMOSPHERES BASED ON THE CN RADICAL EMISSION SPECTRUM

1 State Key Laboratory of High Temperature Gas Dynamics, Institute of Mechanics, Chinese Academy of Sciences, Beijing 100190, China
2 School of Optoelectronics, Beijing Institute of Technology, Beijing 100081, China

Funds: The project was supported by the National Natural Science Foundation of China (11002148, 91216101).

摘要

摘要: 利用氰自由基（CN）B²Σ⁺→X²Σ⁺ 电子带系的发射光谱温度测量技术诊断模拟火星再入流场高温气体的温度. 以双原子分子光谱理论为基础，通过确定CN 自由基B²Σ⁺→X²Σ⁺ 电子带系中 Δv = 0 振动带系发射光谱的跃迁波数、Einstein 跃迁几率以及不同振转能级粒子数等参数，得到了任意转动温度和振动温度下的理论光谱强度分布，结合经窄线宽半导体激光器标定的仪器展宽（Lorentz 线型，半宽度FWHM 为0.154 nm），为CN自由基B²Σ⁺→X²Σ⁺ 电子带系发射光谱测温技术提供理论依据. 利用激波管模拟火星再入流场环境，通过分析激波波后不同时刻处高时间、空间分辨率的CN 自由基发射光谱，得到了激波波后高温气体不同时刻处的转动温度和振动温度，并根据得到的温度信息给出了激波诱导时间和弛豫时间.
- 发射光谱 /
- 谱线强度 /
- 火星再入 /
- 转动温度 /
- 振动温度
Abstract: Temperature measurements behind the strong shock waves for simulated Martian atmosphere were presented in this paper. Based on the inherent molecular structure characteristics of the CN radicals, the energy level distribution, the transition frequency and Einstein spontaneous emission transition probability were systematically analyzed and numerically studied. Meanwhile, the FWHM of apparatus function was measured experimentally to be Lorentzian profile of value 0.154nm by using of a narrow line width diode laser. The dependence of the spectral structure on the rotational temperature and vibrational temperature were numerically analyzed in detailed. In shock-tube experiments, the emission of CN (B²Σ⁺→X²Σ⁺) system measurements were performed behind a strong shock wave in a CO₂-N₂ mixture with two di erent conditions of initial pressure and velocity. Rotational and vibrational temperatures behind the strong shock wave, and the radiation structure of the shock layer, including induction, relaxation and equilibrium processes were obtained through analysis of time gating optical emission spectra with nanosecond temporal resolution.
- emission spectroscopy /
- line intensity /
- Mars re-entry /
- rotational temperature /
- vibrational temperature

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