SOLARNET Conference: The Many Scales of the Magnetic Sun

The multiscale dynamics associated with turbulent magneto-convection in physical systems dominated by very high Rayleigh numbers is a challenged topic in the community of astrophysicists and physicists dealing with heat transport by convection. The Sun represents a unique natural laboratory in which to explore turbulent magneto-convection in the hard turbulence regime, a regime associated to very high values of the Rayleigh number. Flow and heat pattern inside solar plasma allow us to investigate the geometry of solar magneto-convection using photospheric magnetic voids (or simply voids), i.e., photospheric regions nearly devoid of magnetic elements, which cover the whole solar surface and which demarcate the solar magnetic network. In this work we show a large statistical study, involving many spatial scales (1–80 Mm), associated to identified voids in magnetograms acquired during Solar Cycles 23 and 24.