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We describe a model for the thermal and dynamical equilibrium of starlesscores that includes the radiative transfer of the gas and dust and simple COchemistry. The model shows that the structure and behavior of the cores issignificantly different depending on whether the central density is eitherabove or below about 10^5 cm-3. This density is significant as the criticaldensity for gas cooling by gas-dust collisions and also as the critical densityfor dynamical stability, given the typical properties of the starless cores.The starless cores thus divide into two classes that we refer to as thermallysuper-critical and thermally sub-critical.This two-class distinction allows animproved interpretation of the different observational data of starless coreswithin a single model.

The Different Structures of the Two Classes of Starless Cores