  Supernovae feedback driven expansion has proven to be a viable mechanism to
explain the average properties of Ultra Diffuse Galaxies (UDGs) such as the
sizes, colors, mass and internal kinematics. Here, we explore the origin of
stellar metallicity gradients in feedback driven simulated UDGs from the NIHAO
project and compare them with the observed distribution of metallicity
gradients of both Local Group dwarfs as well as of the recently observed UDG
DF44. Simulated UDGs display a large variety of metallicity profiles, showing
flat to negative gradients, similarly to what is observed in LG dwarfs, while
DF44 data suggest a flat to positive gradient. The variety of metallicity
gradients in simulations is set by the interplay between the radius at which
star formation occurs and the subsequent supernovae feedback driven stellar
redistribution: rotation supported systems tend to have flat metallicity
profiles while dispersion supported galaxies show negative and steep profiles.
  Our results suggest that UDGs are not peculiar in what regards their
metallicity gradients, when compared to regular dwarfs. Desirably, a larger
observational sample of UDGs' gradients shall be available in the future, in
order to test our predictions.
