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Numerical simulations of star formation frequently rely on the implementationof sink particles, (a) to avoid expending computational resource on thedetailed internal physics of individual collapsing protostars, (b) to derivemass functions, binary statistics and clustering kinematics (and hence to makecomparisons with observation), and (c) to model radiative and mechanicalfeedback; sink particles are also used in other contexts, for example torepresent accreting black holes in galactic nuclei. We present a new algorithmfor creating and evolving sink particles in SPH simulations, which appears torepresent a significant improvement over existing algorithms {\refrpt --particularly in situations where sinks are introduced after the gas has becomeoptically thick to its own cooling radiation and started to heat up byadiabatic compression}. (i) It avoids spurious creation of sinks. (ii) Itregulates the accretion of matter onto a sink so as to mitigate non-physicalperturbations in the vicinity of the sink. (iii) Sinks accrete matter, but theassociated angular momentum is transferred back to the surrounding medium. Withthe new algorithm -- and modulo the need to invoke sufficient resolution tocapture the physics preceding sink formation -- the properties of sinks formedin simulations are essentially independent of the user-defined parameters ofsink creation, or the number of SPH particles used.

An improved sink particle algorithm for SPH simulations