  We investigate the effect of the turbulent power spectrum (P(k) \propto
k^{-n}, with n=3, 4 or 5) on the fragmentation of low-mass cores, by means of
SPH simulations. We adopt initial density profiles and low levels of turbulence
based on observation, and for each n-value we conduct an ensemble of
simulations with different initial seeds for the turbulent velocity field, so
as to obtain reasonable statistics. We find that when power is concentrated at
larger scales (i.e. for larger n), more protostellar objects form and there is
a higher proportion of low-mass stars and brown dwarfs. This is in direct
contrast with the recent results of Delgado Donate et al., presumably because
they adopted much higher levels of turbulence.
