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In the former case, bright loops appear to rise for a long time, with footpoints separating and the field lines below the bright loops shrinking.
There were bright loops around the center of the active region (labeled 'AR'AR
Bright loops of matter arch and twist like fiery fountains above the surface of this gigantic natural nuclear reactor.
In the latter case, the bright loops cease to rise after a short period of reconnection and become rather stable.
Furthermore, reconstruction of the geometry of bright loops requires methods more advanced than the NLFFF (Aschwanden et al. 2014; Malanushenko et al. 2014).
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3D extrapolation with various alpha values shows that the bright loop near the canceling site was highly non-potential.
A method checking how well the bright loop-top kernel represents the site of hot thermal plasma has been proposed.
We illustrate the observations from 31 March 1997 of a bright loop system above an active region off the northeast limb.
It has been confirmed that hot plasma is situated mainly inside the bright loop-top kernels, where it co-exists with cooler plasma.
In the early stage of the second CME, a bright loop was first observed above the solar limb with height of 0.37 R⊙ in EUV images.
Hence, the brighter loops can have greater influence on the magnetic field.
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