Low mass to intermediate‐mass star‐forming hydrostatic cores in self‐gravitating molecular cloud.

In this study, we present low mass to intermediate‐mass star‐forming hydrostatic cores in a self‐gravitating molecular cloud. Considering that the gravitational energy released during the collapse is the energy difference between the initial and final conditions. According to the virial theorem half the change in gravitational energy goes into internal energy the other half gets radiated away. However, half the change in gravitational energy is not completely (100%) emitted in the form of radiation. Therefore, we impose a dimensionless thermodynamic efficiency factor ϵ (where 0 < ϵ < 1) and quantify it as ϵ=4πRc2σTc4Lgf. Using these preconditions, we formulate equations of mass, density, and radius for the first hydrostatic core and the second hydrostatic core. The model shows there is a close relationship between the first hydrostatic core properties and the prestellar core properties. Moreover, the first hydrostatic core properties can influence the second hydrostatic core formation. [ABSTRACT FROM AUTHOR]