The interchange of H-C-N-O-S volatiles between Earth's interior and the hydrosphere and atmosphere has been the subject of considerable study. Recently, models for early Earth evolution adopt the current level of knowledge into describing of the magma oceans interaction with overlaying atmospheres as efforts have been propelled by the recent discovery of exoplanets with masses similar or exceeding those of Earth's. The speciation and solvation mechanism of H-C-N-O-S volatiles enriching silicate melts has mainly been addressed through the incorporation of charged moieties into the silicate framework. Thus, very little is known about the solubility controls of the molecular H-C-N-O-S species (except maybe for H2O). Meanwhile, there are no experimental data about the solubility of these molecular species in carbonate melts. Because of differing thermodynamic H2O properties, especially the larger partial molar volume of molecular H2O in carbonate melts, we hypothesize that H-C-N-S neutral species are more soluble in carbonate than in silicate melts. We will discuss the dissolution mechanisms of molecular H-C-N-S volatiles in silicate and carbonate melts and present new data from hydrothermal diamond anvil cell experiments characterizing volatile distribution between coexisting melts and fluids as a function of redox state, pH, temperature, and pressure. Results will be used to reevaluate noble gases solubility, assuming that their dissolution in hydrous silicate/carbonate melts follows the same mechanisms as H-C-N-S molecular species. Unraveling the introduction, transport, and storage of H-C-N-S volatiles in the interiors of terrestrial-like planets is profoundly linked to the nature of habitability, the origin of life, and the external evidence of conditions favorable for life.