期刊
ASTROPHYSICAL JOURNAL LETTERS
卷 722, 期 2, 页码 L188-L193出版社
IOP PUBLISHING LTD
DOI: 10.1088/2041-8205/722/2/L188
关键词
Sun: evolution; Sun: granulation; Sun: photosphere; Sun: surface magnetism
资金
- UK Science and Technology Facilities Council (STFC)
- AWE Aldermaston
- Northern Ireland Department for Employment and Learning
- STFC [ST/G004986/1, ST/I00016X/1, ST/F002270/1, PP/E000711/1] Funding Source: UKRI
- Science and Technology Facilities Council [PP/E000711/1, ST/I00016X/1, ST/F002270/1, ST/G004986/1] Funding Source: researchfish
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 one-dimensional intensity profiling, is utilized to identify these structures in the observed and simulated data sets. Both distributions peak at an area of approximate to 45,000 km(2), with a sharp decrease toward 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 inter-granular lanes.
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