Volume 511, February 2010
|Number of page(s)||11|
|Published online||04 March 2010|
Dynamics of isolated magnetic bright points derived from Hinode/SOT G-band observations
IGAM/Institute of Physics, University of Graz, Universitätsplatz 5, 8010 Graz, Austria e-mail: email@example.com
2 Laboratoire d'Astrophysique de Toulouse et Tarbes, UMR5572, CNRS et Université Paul Sabatier Toulouse 3, 57 avenue d'Azereix, 65000 Tarbes, France
3 Astronomical Institute of the Slovak Academy of Sciences, 05960 Tatranská Lomnica, Slovakia
4 Institute of Mathematics, University of Vienna, Nordbergstraße 15, 1090 Wien, Austria
Accepted: 20 November 2009
Context. Small-scale magnetic fields in the solar photosphere can be identified in high-resolution magnetograms or in the G-band as magnetic bright points (MBPs). Rapid motions of these fields can cause magneto-hydrodynamical waves and can also lead to nanoflares by magnetic field braiding and twisting. The MBP velocity distribution is a crucial parameter for estimating the amplitudes of those waves and the amount of energy they can contribute to coronal heating.
Aims. The velocity and lifetime distributions of MBPs are derived from solar G-band images of a quiet sun region acquired by the Hinode/SOT instrument with different temporal and spatial sampling rates.
Methods. We developed an automatic segmentation, identification and tracking algorithm to analyse G-Band image sequences to obtain the lifetime and velocity distributions of MBPs. The influence of temporal/spatial sampling rates on these distributions is studied and used to correct the obtained lifetimes and velocity distributions for these digitalisation effects.
Results. After the correction of algorithm effects, we obtained a mean MBP lifetime of min and mean MBP velocities, depending on smoothing processes, in the range of (1–2) . Corrected for temporal sampling effects, we obtained for the effective velocity distribution a Rayleigh function with a coefficient of . The x- and y-components of the velocity distributions are Gaussians. The lifetime distribution can be fitted by an exponential function.
Key words: Sun: photosphere / magnetic fields / techniques: image processing
© ESO, 2010
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