土卫六日辉中N2 Vegard-Kaplan和其他三重态带发射的产生
Production of N2 Vegard-Kaplan and other triplet band emissions in the dayglow of Titan
摘要：
最近，卡西尼紫外成像光谱仪在土卫六的日光临边观测中发现了N2 Vegard-Kaplan波段的辐射。我们目前的模型计算的各种N2三重态在土卫六的高层大气中的生产。分析产额谱技术被用来计算泰坦大气中的稳态光电子通量，这与卡西尼的CAPS仪器所观察到的一致。考虑电子直接碰撞激发、态间级联和猝灭效应，在统计平衡下计算了N2三重态的布居。计算了各三重态的振动能级密度和各三重态的体积产率。垂直积分的开销强度为相同的日期和照明条件下的UVIS观测报告的N2 VK，1 P，2 P，吴Benesch，和反向第一正带的N2被发现分别为132，114，19，22，和22 R。计算所有N2三重态带发射的每个振动跃迁的顶置强度，其跨越从紫外到红外的更宽的波长光谱。给出了计算的VK带总跃迁和显着跃迁的临边强度。VK辐射在150-190 nm波长范围内的模临强度与Cassini UVIS观测到的模临轮廓吻合得很好。通过使用三种不同的太阳通量模型，即，Solar EUV Experiment，Tobiska（2004）的SOLAR 2000模型，以及Richards等人（2006）的HEUVAC模型。由于S2 K和HEUVAC太阳通量模型的计算N2 VK带强度的边缘强度的峰值是一个因素的1.2和0.9，分别使用SEE太阳EUV通量。
英文摘要：
Recently the Cassini Ultraviolet Imaging Spectrograph has revealed the presence of N2 Vegard-Kaplan band emissions in Titan's dayglow limb observation. We present model calculations for the production of various N2 triplet states in the upper atmosphere of Titan. The Analytical Yield Spectra technique is used to calculate steady state photoelectron fluxes in Titan's atmosphere, which are in agreement with those observed by the Cassini's CAPS instrument. Considering direct electron impact excitation, inter-state cascading, and quenching effects, the population of different levels of N2 triplet states are calculated under statistical equilibrium. Densities of all vibrational levels of each triplet state and volume production rates for various triplet states are calculated in the model. Vertically integrated overhead intensities for the same date and lighting conditions as the reported by UVIS observations for N2 VK, 1P, 2P, Wu-Benesch, and Reverse First Positive bands of N2 are found to be 132, 114, 19, 22, and 22 R, respectively. Overhead intensities are calculated for each vibrational transition of all the triplet band emissions of N2, which span a wider spectrum of wavelengths from ultraviolet to infrared. The calculated limb intensities of total and prominent transitions of VK band are presented. The model limb intensity of VK emission within the 150-190 nm wavelength region is in good agreement with the Cassini UVIS observed limb profile. An assessment of the impact of solar EUV flux on the N2 triplet band emission intensity has been made by using three different solar flux models, viz., Solar EUV Experiment, SOLAR2000 model of Tobiska (2004), and HEUVAC model of Richards et al, (2006). The calculated N2 VK band intensity at the peak of limb intensity due to S2K and HEUVAC solar flux models is a factor of 1.2 and 0.9, respectively, of that obtained using SEE solar EUV flux.
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