Abstract.
Dense pockets of cold, molecular gas preclude the formation of
stars. During their infancy and later phases of evolution, stars
inject considerable energy into the interstellar medium by driving
shocks either due to ionising radiation or powerful winds.
Interstellar shock-waves sweep up dense shells of gas that usually
propagate at supersonic velocities. It is proposed, in this paper,
to examine the possibility of dense structure-formation and
perchance, future stellar wombs, in a molecular cloud shocked by
such a shell. Here I shall discuss results of a self-gravitating,
3-dimensional, high-resolution simulation using the smoothed
particle hydrodynamics.
Key words:ISM: clouds, structure -- hydrodynamics