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Highly turbulent nature of convection on the Sun causes strong multi-scaleinteraction of subsurface layers with the photosphere and chromosphere.According to realistic 3D radiative MHD numerical simulations ubiquitoussmall-scale vortex tubes are generated by turbulent flows below the visiblesurface and concentrated in the intergranular lanes. The vortex tubes cancapture and amplify magnetic field, penetrate into chromospheric layers andinitiate quasi-periodic flow eruptions that generates Alfv\'enic waves,transport mass and energy into the solar atmosphere. The simulations revealedhigh-speed flow patterns, and complicated thermodynamic and magnetic structuresin the erupting vortex tubes. The spontaneous eruptions are initiated anddriven by strong pressure gradients in the near-surface layers, and acceleratedby the Lorentz force in the low chromosphere. In this paper, the simulationdata are used to further investigate the dynamics of the eruptions, theirspectro-polarimetric characteristics for the Fe I 6301.5 and 6302.5 A spectrallines, and demonstrate expected signatures of the eruptions in the Hinode SPdata. We found that the complex dynamical structure of vortex tubes (downflowsin the vortex core and upflows on periphery) can be captured by the Stokes Iprofiles. During an eruption, the ratio of down and upflows can suddenlychange, and this effect can be observed in the Stokes V profile. Also, duringthe eruption the linear polarization signal increases, and this also can bedetected with Hinode SP.

Spectro-Polarimetric Properties of Small-Scale Plasma Eruptions Driven by Magnetic Vortex Tubes