Accretion models of the Saturnian satellite suggest that heating released during late stages of its formation was sufficient to create a warm, dense atmosphere with mass at least 30 times greater then the present value (Lunine and Stevemson, 1983) and large open ocean on its surface. Such juvenile Titan’s ocean could exist during period of 108 years. As the great part of the primordial Titan’s atmosphere could be supplied by comets during or after accretion, the composition of such atmosphere would have consisted of mostly H2O, N2, CO and CO2, since the cometary carbon appears concentrated in the form of CO (ranging from a few to 45% relative to water), CO2 (∼15%) and heavy organic. The mass of volatile acquired by Titan from comets would be expected to be ∼1020-1022 g for COand 1020-1021 g for N (Griffith and Zahnle, 1995). So we can see that the Titan’s primordial atmosphere could be warm, dense and consist of CO2-(CO)-N2.