  We present numerical investigations into three principal properties of the
small-scale dynamo in stably stratified turbulence: the onset criterion, the
growth rate, and the nature of the magnetic field anisotropy in the kinematic
regime. The results suggest that all three dynamo properties are controlled by
the scale separation between the Ozmidov scale and the viscous or resistive
scale. In addition to the critical magnetic Reynolds number, this allows for
the definition of critical buoyancy and magnetic buoyancy Reynolds numbers for
stratified small-scale dynamo onset in the high and low magnetic Prandtl number
regimes, respectively. The presence of a small-scale dynamo in stellar
radiative zones could affect dynamics through resulting Maxwell stresses and/or
influence large-scale dynamo mechanisms in regions of differential rotation.
Taking the solar radiative zone as a representative example and applying the
onset criterion, we find that the stratification is strong enough to make the
small-scale dynamo marginally active in the stably stratified turbulence of the
solar tachocline.
