Filigree, magnetic fields, and flows in the photosphere

Details Filigree, magnetic fields, and flows in the photosphere Filigree, magnetic fields, and flows in the photosphere

Mar 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993soph..144....1y&link_type=abstract

Solar Physics (ISSN 0038-0938), vol. 144, no. 1, p. 1-14.

Physics

23

Photosphere, Solar Granulation, Solar Magnetic Field, Solar Physics, Brightness, Flux Density, Magnetic Flux

Scientific paper

The interaction between small-scale magnetic fields and horizontal photospheric flows has been studied from observations of high angular resolution (1/4 arcsec) obtained with the narrowband filter in the Swedish Vacuum Solar Telescope at La Palma. The measured magnetic flux density (aBII) is in the range from a detection limit of roughly 10 G to about 500 G, showing a good correspondence with the filigree. The magnetic flux elements take part in the local flows towards downdrafts at the supergranulation ceil boundaries. The measured flux density, as well as the associated filigree intensity, decrease as the structures approach the downdrafts, presumably as a result of increased tilting and possibly submergence of flux into the downdrafts.

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