Summary: ARMAGH .
accepted in A&A
The Structure and Dynamics of a Bright Point as seen with Hinode,
SoHO and TRACE
D. PŽerez-SuŽarez1, R.C. Maclean1,3, J.G. Doyle1, and M.S. Madjarska2
Armagh Observatory, College Hill, Armagh BT61 9DG, N. Ireland
Max-Planck-Institut fšur Sonnensystemforschung, Max-Planck-Str. 2, 37191 Katlenburg-Lindau, Germany
now at: School of Mathematics and Statistics, University of St. Andrews, North Haugh, St. Andrews, Fife KY16 9SS, UK
Context. Solar coronal bright points have been studied already for more than three decades but some fundamental questions about
their formation and evolution still remain unanswered.
Aims. Our aim is to determine the plasma properties of a coronal bright point and compare its magnetic topology extrapolated from
magnetogram data with its appearance in X-ray images.
Methods. We analysed spectroscopic data obtained with EIS/Hinode, Ca II H and G-band images from SOT/Hinode, UV images from