Present study deals with the model calculations of CO Cameron band and CO _ { 2 } ^ { + } ultraviolet doublet emissions in the dayglow of Venus .
The overhead and limb intensities of CO Cameron band and CO _ { 2 } ^ { + } UV doublet emissions are calculated for low , moderate , and high solar activity conditions .
Using updated cross sections , the impact of different e-CO cross section for Cameron band production is estimated .
The electron impact on CO is the major source mechanism of Cameron band , followed by electron and photon impact dissociation of CO _ { 2 } .
The overhead intensities of CO Cameron band and CO _ { 2 } ^ { + } UV doublet emissions are about a factor of 2 higher in solar maximum than those in solar minimum condition .
The effect of solar EUV flux models on the emission intensity is \sim 30-40 % in solar minimum condition and \sim 2-10 % in solar maximum condition .
At the altitude of emission peak ( \sim 135 km ) , the model predicted limb intensity of CO Cameron band and CO _ { 2 } ^ { + } UV doublet emissions in moderate ( F10.7=130 ) solar activity condition is about 2400 and 300 kR , respectively , which is in agreement with the very recently published SPICAV/Venus Express observation .
The model limb intensity profiles of CO Cameron band and CO _ { 2 } ^ { + } UV doublet are compared with SPICAV observation .
We also calculated intensities of N _ { 2 } Vegard-Kaplan UV bands and OI 2972 Å emissions during moderate and high solar activity conditions .