The area distribution of solar magnetic bright points

摘要: Magnetic bright points (MBPs) are among the smallest observable objects on solar photosphere. A combination of G-band observations and numerical simulations is used to determine their area distribution. An automatic detection algorithm, employing one-dimensional intensity profiling, utilized identify these structures in observed simulated data sets. Both distributions peak at an ≈45,000 km2, with a sharp decrease toward smaller areas. The conform log-normal statistics, which suggests that flux fragmentation dominates over convergence. Radiative magneto-convection indicate independence MBP distribution for differing magnetic densities. most commonly occurring point size corresponds typical width inter-granular lanes.