Reconnection and Flares: Introduction
Magnetic fields are easily generated in astrophysical plasma owing to its high conductivity. Magnetic fields, having strengths of order few 10-6 G, correlated on several kiloparsec scales are seen in spiral galaxies. Their origin could be due to amplification of a small seed field by a turbulent galactic dynamo. In several galaxies, like the famous M51, magnetic fields are well correlated (or anti-correlated) with the optical spiral arms. These are the weakest large-scale fields observed in cosmic space. The strongest magnets in space are presumably the so-called magnetars, the highly magnetized (with the strength of the field of about 1015 G) young neutron stars formed in the supernova explosions.
KeywordsCoronal Mass Ejection Magnetic Reconnection Solar Atmosphere Spiral Galaxy Astrophysical Plasma
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