  We present the results of an ensemble of SPH simulations that follow the
evolution of prestellar cores for $0.2\,{\rm Myr}$. All the cores have the same
mass, and start with the same radius, density profile, thermal and turbulent
energy. Our purpose is to explore the consequences of varying the fraction of
turbulent energy, $\delta_\mathrm{sol}$, that is solenoidal, as opposed to
compressive; specifically we consider
$\delta_\mathrm{sol}=1,\,2/3,\,1/3,\,1/9\;{\rm and}\;0$. For each value of
$\delta_\mathrm{sol}$, we follow ten different realisations of the turbulent
velocity field, in order also to have a measure of the stochastic variance
blurring any systematic trends. With low $\delta_\mathrm{sol}(<\!1/3)$ filament
fragmentation dominates and delivers relatively high mass stars. Conversely,
with high values of $\delta_\mathrm{sol}(>\!1/3)$ disc fragmentation dominates
and delivers relatively low mass stars. There are no discernible systematic
trends in the multiplicity statistics obtained with different
$\delta_\mathrm{sol}$.
