Astronomy and Astrophysics – Astrophysics
Scientific paper
Sep 1993
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993a%26a...276..236b&link_type=abstract
Astronomy and Astrophysics, Vol. 276, p. 236 (1993)
Astronomy and Astrophysics
Astrophysics
8
Sun: Magnetic Fields, Sun: Photosphere, Mhd, Instabilities
Scientific paper
The geometry of small magnetic flux concentrations in the solar photo sphere lies somewhere between the two extremes of a cylindrical tube and an elongated magnetic slab. A comparison of the two geometries shows that small slabs - like tubes - are unstable to fluting just below continuum optical depth unity (τc = 1), but - unlike tubes - remain unstable deeper down in the convection zone. Whereas tubes may be stabilized by the surrounding intergranular whirl motion, there is no natural mechanism to stabilize a flux sheet against fluting. This suggests that immediately after their formation slabs with diameters ≲ 1000 km are fragmented into tube-filaments below Tc = 1.
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