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).
![](https://s2.save4k.ru/pic/wRc48fIY6Vc/maxresdefault.jpg)