Physics of coronal loops: Heating and reconnection

Details Physics of coronal loops: Heating and reconnection Physics of coronal loops: Heating and reconnection

May 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992esasp.344...69h&link_type=abstract

In ESA, Solar Physics and Astrophysics at Interferometric Resolution p 69-72 (SEE N93-10901 01-90)

Physics

2

Coronal Loops, Magnetic Field Reconnection, Solar Heating, Solar Physics, Field Emission, Fine Structure, Magnetohydrodynamics, Plasma Turbulence

Scientific paper

The importance of small scale structures in the current distribution is outlined, and the smallest size that these current structures might have is discussed. It is shown that they must be dynamic, turbulent structures. The physical processes that may be at the origin of the formation of such structures are discussed. The braiding of field lines, the phase mixing of oscillations in inhomogeneous magnetic configurations, and a number of secondary instabilities are likely to be the dominant ones. A self-consistent calculation of a large scale coronal flow with associated turbulence is described. This parameter free theory gives, as a function of boundary motions which cause it, the rate of coronal heating by fine scaled DC current structures.

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