Filaments and largescale magnetic fields

Details Filaments and largescale magnetic fields Filaments and largescale magnetic fields

May 1995

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995an....316..249m&link_type=abstract

Astronomische Nachrichten v.316:4, P. 249, 1995

Astronomy and Astrophysics

Astronomy

4

Sun: Filaments, Magnetic Fields

Scientific paper

B We have used Stanford magnetic field maps to construct distributions of longitudinal magnetic field gradients in the neighbourhood of polarity inversion lines. The distributions were constructed with proper account of the type of the polarity inversion lines and of the existence or absence of dark filaments above item. It is shown that for polarity inversion lines that pass inside active regions or on their boundary, grad B distributions for portions of the lines with persisting filament are shifted toward lower values of gradient as compared with grad B distributions for portions of the lines without filaments. The influence of the spatial resolution of the magnetogams upon polarity inversion line characteristics is discussed.

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