Interplay of Chemistry and Dynamics in the Low-Mass Star Formation

Cores are subject to gravitational instability; they are massive enough to collapse due to their own gravity. The cores are supported against collapse by a pressure gradient due to the combination of thermal, magnetic, and turbulent pressure. The cores start collapse to form stars, once the gravity overwhelms the pressure gradient. The core before star formation is called a prestellar core, whereas the core harboring protostar(s) are called a protostellar core. Molecular line observations in radio wavelength is a very powerful tool to investigate the core structure, since millimeter radiation suffer much less attenuation than shorter wavelength. High spectral resolution of radio telescopes also enable us to investigate dynamics of the core.