  Using radiative magneto-hydrodynamic simulations of the magnetised solar
photosphere and detailed spectro-polarimetric diagnostics with the FeI
$6301.5\mathrm{\AA}$ and $6302.5\mathrm{\AA}$ photospheric lines in the local
thermodynamic equilibrium approximation, we model active solar granulation as
if it was observed at the solar limb. We analyse general properties of the
radiation across the solar limb, such as the continuum and the line core limb
darkening and the granulation contrast. We demonstrate the presence of profiles
with both emission and absorption features at the simulated solar limb, and
pure emission profiles above the limb. These profiles are associated with the
regions of strong linear polarisation of the emergent radiation, indicating the
influence of the intergranular magnetic fields on the line formation. We
analyse physical origins of the emission wings in the Stokes profiles at the
limb, and demonstrate that these features are produced by localised heating and
torsional motions in the intergranular magnetic flux concentrations.
