The Area Distribution of Solar Magnetic Bright Points

Details The Area Distribution of Solar Magnetic Bright Points The Area Distribution of Solar Magnetic Bright Points

2010-09-13

arxiv.org/abs/1009.2410v1

Astronomy and Astrophysics

Astrophysics

Solar and Stellar Astrophysics

Astrophysical Journal, accepted

Scientific paper

Magnetic Bright Points (MBPs) are among the smallest observable objects on the solar photosphere. A combination of G-band observations and numerical simulations is used to determine their area distribution. An automatic detection algorithm, employing 1-dimensional intensity profiling, is utilized to identify these structures in the observed and simulated datasets. Both distributions peak at an area of $\approx$45000 km$^2$, with a sharp decrease towards smaller areas. The distributions conform with log-normal statistics, which suggests that flux fragmentation dominates over flux convergence. Radiative magneto-convection simulations indicate an independence in the MBP area distribution for differing magnetic flux densities. The most commonly occurring bright point size corresponds to the typical width of intergranular lanes.

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