The photospheric dynamo. I - Magnetic flux-tube generation

Details The photospheric dynamo. I - Magnetic flux-tube generation The photospheric dynamo. I - Magnetic flux-tube generation

Jan 1991

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991a%26a...241..613h&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 241, no. 2, Jan. 1991, p. 613-617.

Astronomy and Astrophysics

Astrophysics

20

Dynamo Theory, Magnetic Flux, Photosphere, Solar Magnetic Field, Magnetic Field Configurations, Sunspots

Scientific paper

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 with 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 the magnetic field from 0.01 G to 1000 G inside thin magnetic flux tubes in the photosphere. The hypothesis of local cooling by advection of ionization energy of Schatten and Mayr (1985) is tested, and it is seen 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. In agreement with recent infrared observations, the inside of the flux-tube is predicted to be cooler than the outside.

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