Astronomy and Astrophysics – Astrophysics
Scientific paper
Mar 1989
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1989apj...338.1148m&link_type=abstract
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 338, March 15, 1989, p. 1148-1157. Research supported by NASA.
Astronomy and Astrophysics
Astrophysics
112
Electric Current, Solar Corona, Solar Prominences, Current Density, Field Strength, Flow Distribution, Magnetohydrodynamics, Photosphere, Solar Magnetic Field
Scientific paper
It has been suggested that the solar corona is heated by the dissipation of electric currents. The low value of the resistivity requires the magnetic field to have structure at very small length scales if this mechanism is to work. In this paper it is demonstrated that the coronal magnetic field acquires small-scale structure through the braiding produced by smooth, randomly phased, photospheric flows. The current density develops a filamentary structure and grows exponentially in time. Nonlinear processes in the ideal magnetohydrodynamic equations produce a cascade effect, in which the structure introduced by the flow at large length scales is transferred to smaller scales. If this process continues down to the resistive dissipation length scale, it would provide an effective mechanism for coronal heating.
Mikic Zoran
Schnack Dalton D.
van Hoven Gerard
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