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I will present numerical simulations of the
interaction between an expanding HII region and an ambient molecular cloud,
illustrating the morphologies of the bright-rimmed cloud structures that
develop, the associated patterns of triggered star formation, and the
statistical properties of the resulting prestellar cores and pre-Main
Sequence stars. I will compare the role played by pre-existing density
structures in the molecular cloud, and the role played by gravitational
instability in the shock-compressed gas which precedes the advancing
ionisation front, in forming prestellar cores. I will also identify the
conditions under which expanding HII regions are ineffectual in triggering
star formation.
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