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Recently, a subset of starless cores whose thermal Jeans mass is apparentlyoverwhelmed by the mass of the core has been identified, e.g., the core {\smallL183}. In literature, massive cores such as this one are often referred to as"super-Jeans cores". As starless cores are perhaps on the cusp of formingstars, a study of their dynamics will improve our understanding of thetransition from the prestellar to the protostellar phase. In the present workwe use non-magnetic polytropes belonging originally to the family of theIsothermal sphere. For the purpose, perturbations were applied to individualpolytropes, first by replacing the isothermal gas with a gas that was cold nearthe centre of the polytrope and relatively warm in the outer regions, andsecond, through a slight compression of the polytrope by raising the externalconfining pressure. Using this latter configuration we identify thermodynamicconditions under which a core is likely to remain starless. In fact, we alsoargue that the attribute "super-Jeans" is subjective and that these cores donot formally violate the Jeans stability criterion. On the basis of our testresults we suggest that gas temperature in a star-forming cloud is crucialtowards the formation and evolution of a core. Simulations in this work wereperformed using the particle-based Smoothed Particle Hydrodynamics algorithm.However, to establish numerical convergence of the results we suggest similartests with a grid-scheme, such as the Adaptive mesh refinement.

Does a prestellar core always become protostellar? Tracing the evolution of cores from the prestellar to protostellar phase