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The bulk of the quiet solar photosphere is thought to be significantlymagnetized, due to the ubiquitous presence of a tangled magnetic field atsubresolution scales with an average strength <B> ~ 100 G. This conclusion wasreached through detailed three-dimensional (3D) radiative transfer modeling ofthe Hanle effect in the Sr I 4607 line, using the microturbulent fieldapproximation and assuming that the shape of the probability density functionof the magnetic field strength is exponential. Here we relax bothapproximations by modeling the observed scattering polarization in terms of theHanle effect produced by the magnetic field of a 3D photospheric modelresulting from a (state-of-the-art) magneto-convection simulation with surfacedynamo action. We show that the scattering polarization amplitudes observed inthe Sr I 4607 line can be explained only after enhancing the magnetic strengthof the photospheric model by a sizable scaling factor, F=10, which implies <B>= 130 G in the upper photosphere. We argue also that in order to explain boththe Hanle depolarization of the Sr I 4607 line and the Zeeman signals observedin Fe I lines we need to introduce a height-dependent scaling factor, such thatthe ensuing <B> = 160 G in the low photosphere and <B> = 130 G in the upperphotosphere.

Determining the Magnetization of the Quiet Sun Photosphere from the Hanle Effect and Surface Dynamo Simulations