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首页> 外文会议>Ultraviolet Technology IV >Electron impact emission cross sections needed in modeling UV observations of the u
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Electron impact emission cross sections needed in modeling UV observations of the u

机译：模拟u的UV观测所需的电子冲击发射截面

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Abstract: In the upper atmospheres and torus regions of the Jovian and Terrestrial planets a dominant mechanism for energy transfer occurs through electron collisional processes with both neutral and ionic species leading to UV radiation. In response to the need for accurate collision cross sections to model spectroscopic observations of planetary systems and calibrate flight instruments, JPL has measured in the laboratory emission cross sections of H, H$-2$/ N$-2$/, and SO$-2$/ and other important planetary gases. Voyager and International Ultraviolet Explorer (IUE) spacecraft have established that band systems of H$-2$/ and N$-2$/ are the dominant UV molecular emissions in the solar system produced by electron impact. The threshold energy cross section behavior (0 - 100 eV) and spectra of H$-2$/ and N$-2$/ are complex because of configuration interaction among states in the 8 - 14 eV energy range. Resonance excitation, predissociation and non-Franck-Condon band intensities systems are a consequence of configuration interaction and must be considered in analyzing spacecraft observations. Applications of our cross section data to electron energy loss codes and to models of Voyager, IUE, Galileo, and Hubble Space Telescope (HST) observations of the planets are described. !30
机译：摘要：在木星和陆地行星的高层大气和圆环区域，能量转移的主要机制是通过电子碰撞过程发生的，其中中性和离子物种均会导致紫外线辐射。为满足对精确碰撞截面进行建模以对行星系统和校准飞行仪器进行光谱观测建模的需求，JPL在实验室排放截面中测量了H，H $ -2 $ / N $ -2 $ /和SO $ -2 $ /和其他重要的行星气体。 Voyager和国际紫外线探测器（IUE）航天器已经确定，H $ -2 $ /和N $ -2 $ /的波段系统是电子撞击产生的太阳系中主要的UV分子发射。 H $ -2 $ /和N $ -2 $ /的阈值能量截面行为（0-100 eV）和光谱很复杂，因为在8-14 eV能量范围内的状态之间存在构型相互作用。共振激发，预离解和非弗朗克-康登带强度系统是构型相互作用的结果，在分析航天器观测结果时必须加以考虑。描述了我们的横截面数据在电子能量损失代码以及行星的Voyager，IUE，Galileo和哈勃太空望远镜（HST）观测模型中的应用。 ！30

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