The association of chromospheric and coronal phenomena with the evolution of the quiet sun magnetic fields

Details The association of chromospheric and coronal phenomena with the evolution of the quiet sun magnetic fields The association of chromospheric and coronal phenomena with the evolution of the quiet sun magnetic fields

Dec 1986

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986nascp2442..359h&link_type=abstract

In NASA. Goddard Space Flight Center Coronal and Prominence Plasmas p 359-363 (SEE N87-20871 13-92)

Physics

4

Magnetic Flux, Solar Activity, Solar Cycles, Solar Granulation, Sun, Line Spectra, Magnetic Signatures, Polarity, Spectroheliographs

Scientific paper

Using daily full-disk magnetograms and He I 10830 spectroheliograms to study the count and surface distribution of ephemeral regions over the solar cycle, Harvey (1985) concluded that the small dark structures seen in 10830, thought to correspond to X-ray bright points, were more often associated with magnetic bipoles that appeared to result from an encounter of already existing opposite polarity magentic flux than with emerging small magnetic bipoles (ephemeral regions). Such encounters would be more likely to occur in areas of mixed polarity. The fractional area of the sun covered by mixed polarity fields varies anti-correlated with the solar cycle leading to a possible explanation for the 180 degrees out of phase solar cycle variation of X-ray bright points. To establish the validity of this suggestion, a detailed study of time-sequence magnetic field, He I wavelength 10830, Ha, C IV, and Si II observations of selected areas of the quiet sun was initiated about 2 years ago. The preliminary results of this study are reported.

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