Dayglow Emissions on Mars and Venus

An attempt has been made in this thesis to model some of the emissions observed by SPICAM and SPICAV on Mars and Venus, respectively, viz., CO Cameron band, CO+ 2 ultraviolet doublet, N2 triplet bands, atomic oxygen green (5577 A), red doublet (6300, 6364 A), and ultraviolet (2972 A) emissions. One of major sources of these emissions is photoelectron impact ionization/excitation. In this thesis, an electron degradation model based on Monte Carlo technique has been developed to calculate the production/excitation rates of above mentioned emissions due to electron impact. The limb brightness pro les of emissions are calculated and compared with the observations wherever available. The e ect of various model input parameters on dayglow emissions intensities is also evaluated