Coronal Condensations Caused by Magnetic Reconnection between Solar Coronal Loops

Magnetic reconnection in kinked coronal loops

The resistive dissipation process triggered by the non linear development of the kink instability in a coronal loop is investigated using a three-dimensional MHD code in cylindrical geometry. An equilibrium flux tube carrying a zero net axial current is considered. The magnetic field lines are locally twisted in the central region and inertially anchored at the two photospheric end-plates. When...

Relating magnetic reconnection to coronal heating.

It is clear that the solar corona is being heated and that coronal magnetic fields undergo reconnection all the time. Here we attempt to show that these two facts are related--i.e. coronal reconnection generates heat. This attempt must address the fact that topological change of field lines does not automatically generate heat. We present one case of flux emergence where we have measured the ra...

Reconstruction of Solar Coronal Linear Force-Free Magnetic Field

Nonlinear wave heating of solar coronal loops

Theheating ofmagnetically closed structures (loops) in the solar corona by the resonant absorption of incident waves is studied by means of numerical simulations in the framework of nonlinear resistive magnetohydrodynamics (MHD). It is shown that the dynamics in the resonant layer is indeed very nonlinear for typical coronal parameters. The effect of the nonlinearity on the efficiency of the re...

Observations of Solar Coronal Magnetic

This review discusses methods for determining solar coro-nal magnetic elds, with an emphasis on radio measurements of eld strengths in solar active regions.