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One of the key research problems in stellar physics is to decipher thesmall-scale magnetic activity of the quiet solar atmosphere. Recentmagneto-convection simulations that account for small-scale dynamo action haveprovided three-dimensional (3D) models of the solar photosphere characterizedby a high degree of small-scale magnetic activity, similar to that foundthrough theoretical interpretation of the scattering polarization observed inthe Sr I 4607 \AA\ line. Here we present the results of a novel investigationof the Hanle effect in this resonance line, based on 3D radiative transfercalculations in a high-resolution magneto-convection model having most of theconvection zone magnetized close to the equipartition and a surface mean fieldstrength ${\langle B \rangle}{\approx}170$ G. The Hanle effect produced by themodel's magnetic field depolarizes the zero-field scattering polarizationsignals significantly, to the extent that the center-to-limb variation of thecalculated spatially-averaged polarization amplitudes is compatible with theobservations. The standard deviation of the horizontal fluctuations of thecalculated scattering polarization signals is very sensitive to the model'smagnetic field and we find that the predicted spatial variations aresufficiently sizable so as to be able to detect them, especially with the nextgeneration of solar telescopes. We find that at all on-disk positions thetheoretical scattering polarization signals are anti-correlated with thecontinuum intensity. To facilitate reaching new observational breakthroughs, weshow how the theoretically predicted polarization signals and spatialvariations are modified when deteriorating the signal-to-noise ratio and thespectral and spatial resolutions of the simulated observations.

A novel investigation of the small-scale magnetic activity of the quiet Sun via the Hanle effect in the Sr I 4607 \AA\ line