Stars in clusters evolve, and this evolution provides a crucial
feedback on the evolution of the cluster as a whole - through mass
loss, interaction, and collisions between stars. Conversely, the
dynamical cluster environment strongly modifies the evolution of many
of its members, and the often exotic stars that result can be an
important diagnostic of the (hydro)dynamical processes that take
place.
Our challenge is to model the evolution of any star that can be
present in a dense cluster, whether single, binary or a member of a
higher-order multiple. This includes non-canonical stars that result
from stellar mergers and collisions. We thus require a stellar
evolution code that can run autonomously from an arbitrary initial
configuration to the end of a star's nuclear and thermal
evolution. The code should be sufficiently fast so as not grind a
cluster simulation to a halt. Above all, it should be robust and give
a meaningful result under any conceivable circumstance.
| WG home page: | WG2 |
| Contact: | Onno Pols |