Given their small sizes, the cores of meteorite parent bodies likely crystallized inwardly from their core-mantle boundary (CMB). However, the iron snow model of dynamo generation that has been associated with Ganymede and Mars may not apply to these cores. This difference originates from the small adiabatic temperature difference between the CMB and interior of asteroids cores that may prevent remelting of the iron snow, removing the buoyancy source that could drive a dynamo field. Motivated by this, we have developed a set of analogue tank experiments to investigate the iron snow mode of core crystallization in asteroid cores. We find that the mean convective speeds of the fluid increase by approximately a factor of 2 when the fluid crystallizes. This increase in speed is driven by an increase in the bulk density of the fluid in the snow zone due to the presence of a small, entrained crystal fraction. We use our results to explore whether this mechanism can explain the records of dynamo activity recovered from paleomagnetic measurements of meteorites. We show that this mechanism can generate a similar magnitude of turbulence to the remelting-driven iron snow models, making it a possible dynamo mechanism for asteroid cores. Moreover, we consider the caveats of this mechanism, including the potential absence of a stably stratified snow zone and its dependence on crystal size. Finally, we highlight the experimental difficulty in inducing nucleation of solids away from a solid substrate, an observation which should be considered in future iron snow models.