Magnetic network dynamics in photosphere

In order to investigate the interaction between the photospheric velocity field and emerging magnetic elements, observations with high spectral and temporal resolution and with a spatial scale of about 100 km on the solar surface are necessary. The convective advection of magnetic elements produces the magnetic network which is a key component of solar irradiance and of the energy transport toward the solar upper atmosphere. Furthermore, the magnetic network structures are suspected to be the roots of solar wind emanating from localized regions along boundaries of magnetic network cells. We present the results of the preliminary analysis of observations carried out with the panoramic monochromator IBIS, installed at the Dunn Solar Telescope, Sacramento Peak (NM), in the spectral lines Ca II 854.2 nm, Fe I 709.0 nm, and Fe II 722.4 nm.