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=1987cha%26a..11..221s&link_type=abstract

Chinese Astronomy and Astrophysics, Volume 11, Issue 3, p. 221-228.

Astronomy and Astrophysics

Astrophysics

Scientific paper

There are 4 types of evolution patterns of network magnetic fields: (1) flux cancellation, the mutual disappearance of encountering fluxes of opposite polarity, (2) flux increase by emergence of ephemeral regions, (3) flux decrease of one polarity and (4) flux increase of one polarity, without emergence of ephemeral regions.
From a time sequence of magnetograms of a quiet region of 1983 October 14, the evolution of 300 network features was measured. The magnetograms have a spatial resolution of 2 to 3 arcsec and a time resolution of about 2 hr. The statistics show that the contribution to flux decrease by Type 3 is 1.28 times that by Type 1, and the contribution to flux increase by Type 4 is 7 times that by Type 2.

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