大气压下介质表面闪络自产真空紫外线辐射的探索

G. Laity, A. Fierro, L. Hatfield, A. Neuber
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引用次数: 4

摘要

本文介绍了近年来研究脉冲大气等离子体结构中自产真空紫外(VUV)发射的实验。虽然传统上认为光电离在快速时间尺度(即流光)的等离子体产生中起着重要作用,但VUV辐射(能量大于7 eV)的确切作用直到最近才被探索,目前是航空航天界开发高功率器件的一个感兴趣的领域。由于VUV辐射被分子氧和大多数光学材料大量吸收,直接观测由大气压等离子体产生的VUV辐射具有挑战性。实验在德克萨斯理工大学进行,使用多个真空单色仪,定制设计的VUV透明光学仪器,VUV敏感增强CCD和光电倍增管时间分辨诊断,以及纳秒级等离子体电探针。由于用于紫外传输的聚焦光学的非线性,先前的研究受到限制,因此当前的实验旨在最大限度地减少在感兴趣的紫外波段(115 - 135 nm)记录发射的色像差。对空气中表面闪络的紫外辐射进行了定量观测,结果表明,在130 ~ 135 nm波长范围内,绝大部分紫外辐射来自原子氧和原子氮的辐射,这一结果在玻耳兹曼温度为10 eV的条件下得到了光谱计算的证实。在115 - 130 nm范围内的高分辨率光谱测量也导致沿表面观察到各种杂质,这些杂质只能通过升级的聚焦系统才能观察到。最后,时间分辨测量表明,最早的VUV发射发生在拖缆阶段,由于更有效的光学诊断,在此阶段观测到的发射的记录信噪比显着增加。
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Exploration of self-produced vacuum ultraviolet radiation from dielectric surface flashover at atmospheric pressure
This paper describes recent experiments to study selfproduced vacuum ultraviolet (VUV) emission from pulsed atmospheric plasma structures. While it has been classically believed that photo-ionization plays a significant role on plasma generation during fast timescales (i.e. streamers), the exact role of VUV radiation (energy greater than 7 eV) has only recently been explored and is currently an area of interest for the development of high power devices in the aerospace community. Since VUV emission is heavily absorbed by molecular oxygen and most optical materials, the direct observation of VUV radiation produced by atmospheric pressure plasmas is challenging. Experiments at Texas Tech University were performed with multiple vacuum monochromators, custom designed VUV transparent optical instruments, VUV sensitive intensified CCD and photomultiplier time-resolved diagnostics, and nanosecondtimescale electrical probes of the plasma. Previous studies were limited due to the non-linearity of the focusing optics used for VUV transmission, and thus the current experiment was designed to minimize chromatic abberation of recorded emission in the VUV regime of interest (115 – 135 nm). Quantitative observation of VUV emission from surface flashover in air revealed that the majority of emission is due to radiation from atomic oxygen and nitrogen in the wavelength range 130 – 135 nm, which has been confirmed by spectral calculation for an estimated Boltzmann temperature of 10 eV. High resolution spectral measurements in the range 115 – 130 nm also led to observation of various impurities along the surface, which were only observable due to the upgraded focusing system. Finally, time resolved measurements showed that the earliest VUV emission occurs during the streamer phase, where the recorded signal-to-noise ratio of the observed emission has been significantly increased due to more efficient optical diagnostics.
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