Description
(Text)
The fine structure of the magnetic field in the solar photosphere is the result of the complex interactions between the magnetic field and convection. Although the spatial resolution of the instruments used in the study of the photospheric magnetic field has improved significantly, a sizeable fraction of the magnetic features remains unresolved even in observations with the currently highest resolution. Realistic magnetohydrodynamic (MHD) numerical models of solar surface layers have reached a level of realism and accuracy that enables a quantitative comparison with observations. The simulations prove to be useful guides for the analysis and interpretation of observations, since they can provide insight into the complex interaction between magnetic field and convection at length scales and depths not accessible to observations. In this thesis, the spectropolarimetric signals synthesized from 3D radiative MHD simulations are compared with observational data acquired with the Spectropolarimeter onboard Hinode satellite. First, theoretical Point Spread Function is constructed that properly takes into account the instrumental effects. Then, questions related to the characteristics of the granulation and the internetwork magnetic field are addressed. Examples of formation and cancellation of the magnetic concentrations in the simulations are shown. Possible observational signatures of the processes and the effects of spatial smearing are considered. A possible role of the surface dynamo in the quiet Sun magnetism is discussed and the amount of magnetic flux contained in the internetwork is estimated.
