About this Research Topic
Following the Big-Bang, isotopes of hydrogen and helium were produced along with some trace amounts of other light elements. The universe grew rapidly and became cold. The atomic gas began to accrete forming large cosmic structures and triggering the formation of stars. The heavier elements were then produced and released in the interstellar medium (ISM) through the various stages of stellar evolution. Here, where favourable physical conditions are met, atoms combined to form larger and larger chemical systems.
Till date, more than 200 species (starting from simple hydrogen molecule to exotic species like, ArH+, HeH+ and pretty big molecules such as, C60, C70, etc.) have been discovered in ISM and numerous complex organic species have been discovered in comets and meteorites which are believed to be formed in the molecular cloud during the early stages of the star formation process. The chemical and dynamical evolution of these regions are highly interrelated. Since molecules are everywhere, these are regularly used to inspect the prevailing conditions. In this issue, we would like to address some of the following topics related to Astrochemistry:
1. Chemical evolution of the star-forming regions and circumstellar envelopes
2. Astrochemical modeling
3. Experimental studies supporting the interpretation of the observations
4. Interstellar dust and ices, structure and chemical composition and their role in gas-grain chemistry
5. Formation of complex organic molecules in space from gas-phase and gas-grain chemistry
Keywords: Astrochemistry, Interstellar molecules, Star-formation, Interstellar Dust, Complex organic molecules
Important Note: All contributions to this Research Topic must be within the scope of the section and journal to which they are submitted, as defined in their mission statements. Frontiers reserves the right to guide an out-of-scope manuscript to a more suitable section or journal at any stage of peer review.