Astronomy and Astrophysics – Astronomy
Scientific paper
Jun 1993
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993soph..145..207d&link_type=abstract
Solar Physics (ISSN 0038-0938), vol. 145, no. 2, p. 207-225.
Astronomy and Astrophysics
Astronomy
196
Dynamo Theory, Magnetohydrodynamic Turbulence, Solar Convection (Astronomy), Solar Magnetic Field, Stellar Interiors, Chromosphere, Helices, Poloidal Flux, Solar Radiation, Stellar Rotation
Scientific paper
The generation of large-scale solar-cycle magnetic fields at the interface of the radiative core and the solar convection zone (SCZ) is discussed. It is shown that the SCZ actively generates a small-scale turbulent magnetic field. An argument is presented for the existence of three distinctive components of the residual chromospheric emission. The turbulent magnetic field is discussed and global wave pattern decomposition of the solar magnetic field is examined. Solar dynamo theories are reviewed and it is suggested that the surface layers may be essential for generation of the poloidal field. It is concluded that the chromospheric emission of fully convective stars may be explained by the generation of a small-scale turbulent magnetic field in late-type stars.
de Young David S.
Durney Bernard R.
Roxburgh Ian W.
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