Astronomy and Astrophysics – Astrophysics
Scientific paper
Jun 1994
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994a%26a...286..275g&link_type=abstract
Astronomy and Astrophysics 286, 275-301 (1994)
Astronomy and Astrophysics
Astrophysics
37
Mhd, Waves, Sun: Corona, Sun: Magnetic Fields
Scientific paper
The problem of the basic MHD waves of a coronal flux loop is investigated for the simplest configuration conceivable, viz. a plasma in a rectangular box, with an oblique magnetic field, and line-tied at the ends. The basic waves found are completely different from those found in a periodic box, representative for tokamak plasmas. They consist of an interwoven structure of Alfven and slow components with a ballooning factor, favouring minimal field line bending, and fast components without such a factor. The implications for stability are the existence of a global excess of stability in coronal loops, as opposed to local marginal stability at rational magnetic surfaces in tokamaks. The relationship to flares is pointed out. Pure Alfven and pure slow modes are only found as singular limiting cases of cluster spectra of Alfven-fast or slow-fast waves, where the fast components are localised in a photospheric boundary layer which is dictated by the requirements of line-tying. This justifies the assumption of continuous spectra in coronal loops, required for the mechanism of resonant Alfven wave heating. The waves consist of large amplitude Alfven components in the corona and fast components with a small but rapidly varying amplitude in the photospheric boundary layer, so that they appear to have all the right characteristics for effective transfer of energy from the photosphere to the corona.
Goedbloed J. P.
Halberstadt G.
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