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A model for N2 triplet states band emissions in the Venusian dayglow has beendeveloped for low and high solar activity conditions. Steady statephotoelectron fluxes and volume excitation rates for N2 triplet states havebeen calculated using the Analytical Yield Spectra (AYS) technique. Modelcalculated photoelectron flux is in good agreement with Pioneer VenusOrbiter-observed electron flux. Since inter-state cascading is important forthe triplet states of N2, populations of different levels of N2 triplet statesare calculated under statistical equilibrium considering direct electron impactexcitation, and cascading and quenching effects. Densities of all vibrationallevels of each triplet state are calculated in the model. Height-integratedoverhead intensities of N2 triplet band emissions are calculated, the valuesfor Vegard-Kaplan (A^3Sigma_u^+ - X^1Pi_g^+), First Positive (B^3Pi_g -A^3Sigma_u^+), Second Positive (C^3Pi_u - B^3Pi_g), and Wu-Benesch (W^3Delta_u- B^3Pi_g) bands of N2, are 1.9 (3.2), 3 (6), 0.4 (0.8), and 0.5 (1.1) kR,respectively, for solar minimum (maximum) conditions. The intensities of thethree strong Vegard-Kaplan bands (0, 5), (0, 6), and (0, 7) are 94 (160), 120(204), and 114 (194) R, respectively, for solar minimum (maximum) conditions.Limb profiles are calculated for VK (0, 4), (0, 5), (0, 6) and (0, 7) bands.The calculated intensities on Venus are about a factor 10 higher than those onMars. The present study provides a motivation for a search of N2 triplet bandemissions in the dayglow of Venus.

Calculations of N2 triplet states vibrational populations and band emissions in Venusian dayglow