The bodies in any N-body system can change. The most changeable bodies are stars. In order to fully model the evolution of a cluster of stars, we need to know how they interact with their environment, particularly how much mass they lose, and how they interact with each other. Is their evolution affected by a companion or close encounter? In this chapter we describe the physics and the mathematical formulation that we use to describe it. If we could we would evolve each star in every detail (Church, Tout & Aarseth 2007) but up to now, in practice, we have had to approximate the detailed evolution by empirical models (Hurley, Tout & Pols 2000).
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Tout, C.A. (2008). Stellar Evolution. In: Aarseth, S.J., Tout, C.A., Mardling, R.A. (eds) The Cambridge N-Body Lectures. Lecture Notes in Physics, vol 760. Springer, Dordrecht. https://doi.org/10.1007/978-1-4020-8431-7_9
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