Abstract Velocities of electrons, ions and neutrals are computed, in the three-fluid approximation, for an axisymmetrical magnetic field. By prescribing a radial dependence of the velocity of neutrals, in agreement whith a downflow, the radial dependence of the magnetic field energy density is derived. This gives the radial flux of neutrals that is required to increase, in the photosphere, the magnetic field from 5 Gauss to 1000 Gauss. We test the hypothesis of local cooling by advection of ionization energy of Schatten and Mayr/1/, and find that this flux of neutrals is high enough to affect significantly the energy balance in the tube and to maintain the pressure gradient necessary to produce the radial inflow of neutrals. The product of the tube radius by the radial velocity V r,n r being, in the photosphere (τ 5000 = 1), lower than a few 105 m.2 s.−1, the associated velocity would presumably not exceed a few meters per second. This supports the idea of creation of strong fields by enhancement of a preexisting magnetic field in the photosphere, i.e. superficial creation of magnetic fluxtubes.
Electrodynamic conversion of energy: Magnetic field amplification in the solar photosphere
Advances in Space Research ; 10 , 9 ; 179-183
1990-01-01
5 pages
Article (Journal)
Electronic Resource
English
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