Projected density, temperature and star particle distribution of a spherical cloud of cold dense (n=100 cm**-3, r=50 pc) gas, undergoing collapse which triggers star formation. Stars more massive than 8 solar masses are treated on a star-by-star basis. This is a highly idealized case to show how my model behaves.

The top panel shows a model giving these stars velocity kicks to mimic the collisional dynamics of the stars which are unresolved in our simulations, while the lower panel shows a model ignoring this mechanism. This produces a population of runaway stars.

For details on the model see Andersson et al. (in prep).

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