A fast and accurate method to compute the mass return from multiple
  stellar populations
  The mass returned to the ambient medium by aging stellar populations over
cosmological times sums up to a significant fraction (20% - 30% or more) of
their initial mass. This continuous mass injection plays a fundamental role in
phenomena such as galaxy formation and evolution, fueling of supermassive black
holes in galaxies and the consequent (negative and positive) feedback
phenomena, and the origin of multiple stellar populations in globular clusters.
In numerical simulations the calculation of the mass return can be time
consuming, since it requires at each time step the evaluation of a convolution
integral over the whole star formation history, so the computational time
increases quadratically with the number of time-steps. The situation can be
especially critical in hydrodynamical simulations, where different grid points
are characterized by different star formation histories, and the gas cooling
and heating times are shorter by orders of magnitude than the characteristic
stellar lifetimes. In this paper we present a fast and accurate method to
compute the mass return from stellar populations undergoing arbitrarily
complicated star formation histories. At each time-step the mass return is
calculated from its value at the previous time, and the star formation rate
over the last time-step only. Therefore in the new scheme there is no need to
store the whole star formation history, and the computational time increases
linearly with the number of time-steps.
