Molecular clouds consisting of gas and dust give birth to stars and surround them are primitive planetary disks that are the mother of the planets. The playground of structural formation from molecular clouds to primitive planetary disk formation is also for molecular evolution, where chemical reactions occur very actively. In particular, understanding elementary surface processes (adsorption, diffusion, desorption, and decomposition) of molecules on dust surfaces is crucial to understanding the full extent of molecular evolution. In traditional interstellar chemistry, theories have been constructed using models based on physically simple assumptions in cryogenic environments. However, recent observations have shown that chemical diversity in molecular clouds has been transferred to the planetary system formation region, and further chemical processes occur. Therefore, observations point out the importance of a rich chemical reaction process resulting from thermal excitation from cryogenic to intermediate (10–300 K), and understanding based on the nature of matter and molecular scientific knowledge is becoming essential. This study aims to reconstruct the theory of material evolution in the universe by using real-space observation and surface spectroscopy at single molecular and atomic levels to reconstruct the basic theory of surface reactivity in a wide range of temperatures from cryogenic to intermediate temperatures.