Evolution of network magnetic fields of solar quiet regions

Details Evolution of network magnetic fields of solar quiet regions Evolution of network magnetic fields of solar quiet regions

Sep 1987

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987acasn..28..111s&link_type=abstract

(Acta Astronomica Sinica, vol. 28, no. 2, 1987, p. 111-119) Chinese Astronomy and Astrophysics (ISSN 0275-1062), vol. 11, Sept.

Astronomy and Astrophysics

Astrophysics

1

Radiant Flux Density, Solar Activity, Solar Magnetic Field, Magnetic Signatures, Spatial Resolution, Statistical Analysis

Scientific paper

The evolution of 300 quiet-region network features is followed in a time series of longitudinal magnetograms obtained (with spatial resolution 2-3 arcsec and time resolution about 2 h) using the VMG at Big Bear Solar Observatory on October 10-14, 1983. The results are presented in sample magnetograms and tables of numerical data. Four general evolution patterns are identified: (1) flux cancellation, (2) flux increase associated with the emergence of ephemeral regions, (3) one-polarity flux decrease, and (4) flux increase in one polarity without emergence of ephemeral regions. Patterns (3) and (4) are shown to be the dominant forms of decrease and increase, respectively.

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