Titan's atmosphere contains some low and high molecular weight hydrocarbons, belonging to the Polyacetylene family (PA) CxH2 (x=2n, n = 1,…,N1), Vinylacetylene family (VA) CxHx (x=2n, n = 1,…,N2), Polyvinyl family (PV) CxHx+2 (x=2n, n = 1,…,N3) up to C60 and a small amount of Allenes CxHx+4. (x=2n, n <5). These species are formed by primary CH4 photolysis and further conversion of the primary products. In this paper we derive the physico-chemical (density, temperature of phase transformation, surface tension, etc.) and thermodynamic (heat-capacity, enthalpy, entropy, etc.) properties of these species by a unified approach, based on their elemental and functional structure. About 200 individual chemical hydrocarbons, both known and unknown (hypothetical), were kept under regular examination. The calculated data were compared, whenever possible, with available information and the accuracy of estimation was found to be satisfactory (~30%). The values of recommended indices (more than 1000 items) can be found in three figures and a table in a condensed form. This information is relevant both for the design of an Adequate Kinetic Model of the chemical pattern in Titan's atmosphere, possible condensation of hydrocarbons into aerosols, to describe the environments the Cassini-Huygens probe will encounter during its descent through the atmosphere and landing on Titan's surface or in the ocean. It may also be relevant for the analysis of low-temperature conversion of acetylene and methane.
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