The classical novae are close binary systems with a late-type main sequence star (the secondary) transferring material via Roche lobe overflow to a companion star (the primary). Novae brighten by 10 - 12 magnitudes in a few hours and subsequently fade back to the original faint level over a period lasting several months to years. The results obtained from the IR observations will be presented. The system parameters of the observed novae, like the distance to the nova, absolute magnitude, expansion velocity of the ejecta, mass of the ejecta and gas to dust ratio are estimated. The dust formation and the detection of first overtone emission bands of CO in these novae will be discussed.