The Area Distribution of Solar Magnetic Bright Points

P. J. Crockett, M. Mathioudakis, D. B. Jess, S. Shelyag, F. P. Keenan, D. J. Christian

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Abstract

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.
Original languageEnglish
Pages (from-to)L188-L193
JournalThe Astrophysical Journal. Letters
Volume722
Early online date01 Oct 2010
DOIs
Publication statusPublished - 20 Oct 2010

ASJC Scopus subject areas

  • Space and Planetary Science
  • Astronomy and Astrophysics

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