Abstract
We review the physical processes and the numerical simulations, which have been performed to address the question of the formation of stellar clusters. Starting with a description of hydrodynamical and isothermal simulations, we then discuss and describe the influence of the radiative feedback, magnetic field, ionising radiation and protostellar jets. Each of these processes has recently been introduced in simulations of cluster formation and turn out to play a significant role, by reducing the star formation efficiency or the star formation rate, or by influencing the shape of the initial mass function. In each case, we start the discussion by describing the most important effects, which are expected and give the relevant analytical expressions, which have been inferred. We then discuss the numerical simulations, which have been performed to investigate their effects.
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