The Area Distribution of Solar Magnetic Bright Points
Data(s) |
20/10/2010
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Resumo |
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. |
Formato |
application/pdf |
Identificador | |
Idioma(s) |
eng |
Direitos |
info:eu-repo/semantics/openAccess |
Fonte |
Crockett , P J , Mathioudakis , M , Jess , D B , Shelyag , S , Keenan , F P & Christian , D J 2010 , ' The Area Distribution of Solar Magnetic Bright Points ' The Astrophysical Journal. Letters , vol 722 , pp. L188-L193 . DOI: 10.1088/2041-8205/722/2/L188 |
Palavras-Chave | #/dk/atira/pure/subjectarea/asjc/1900/1912 #Space and Planetary Science #/dk/atira/pure/subjectarea/asjc/3100/3103 #Astronomy and Astrophysics |
Tipo |
article |