  All cool main sequence stars including our Sun are thought to have magnetic
fields. Observations of the Sun revealed that even in quiet regions small-scale
turbulent magnetic fields are present. Simulations further showed that such
magnetic fields affect the subsurface and photospheric structure, and thus the
radiative transfer and emergent flux. Since small-scale turbulent magnetic
fields on other stars cannot be directly observed, it is imperative to study
their effects on the near surface layers numerically. Until recently
comprehensive three-dimensional simulations capturing the effect of small-scale
turbulent magnetic fields only exists for the solar case. A series of
investigations extending SSD simulations for other stars has been started. Here
we aim to examine small-scale turbulent magnetic fields in stars of solar
effective temperature but different metallicity. We investigate the properties
of three-dimensional simulations of the magneto-convection in boxes covering
the upper convection zone and photosphere carried out with the MURaM code for
metallicity values of $ \rm M/H = \{-1.0, 0.0, 0.5\}$ with and without a
small-scale-dynamo. We find that small-scale turbulent magnetic fields enhanced
by a small-scale turbulent dynamo noticeably affect the subsurface dynamics and
significantly change the flow velocities in the photosphere. Moreover,
significantly stronger magnetic field strengths are present in the convection
zone for low metallicity. Whereas, at the optical surface the averaged vertical
magnetic field ranges from 64G for M/H = 0.5 to 85G for M/H = -1.0.
