The detailed analysis of airglow and auroral optical emission measurements requires sophisticated computer models of electron impact energy loss/excitation processes, photochemistry, and radiative transfer of optically thick EUV resonance lines in the atmosphere. Due to the complexity of the modeling effort, only one group (R.R. Meier and colleagues at NRL) has previously been engaged in comprehensive modeling of the UV spectrum of the dayglow and aurora. In addition to collaborating with Dr. Meier in the analysis of U.C. Berkeley SRP78-1 EUV data, we are now conducting or own theoretical investigations and analyses of both EUV and visible region airglow and aurora. The quantitative investigation of airglow and auroral excitation and emission processes plays a significant role in the elucidation of the photochemistry and energetics of the coupled magnetosphere-ionosphere-atmosphere system. The daytime ionosphere is formed and maintained through the absorption of solar EUV radiation at wavelengths below 1025 . In the auroral zones, where geomagnetic storms may have a profound influence on neutral atmospheric and ionospheric structure, much of the energy deposited in the atmosphere by precipitating energetic electrons is released in the form of optical emissions. Thus, the spectroscopy of atmospheric emissions serves as an important diagnostic tool in understanding and monitoring the global terrestrial environment.
