  Using numerical simulations of the magnetised solar photosphere and radiative
diagnostics of the simulated photospheric models, we further analyse the
physical nature of magnetic photospheric intergranular vortices. We confirm the
magnetic nature of the vortices and find that most MHD Umov-Poynting flux is
produced by horizontal vortex motions in the magnetised intergranular lanes. In
addition, we consider possible ways to directly observe photospheric magnetic
vortices using spectropolarimetry. Although horizontal plasma motions cannot be
detected in the spectropolarimetric observations of solar disk centre, we find
an observational signature of photospheric vortices in simulated observations
of Stokes-V amplitude asymmetry close to the solar limb. Potential ways to find
the vortices in the observations are discussed.
