Variability of the quiet photospheric network

Details Variability of the quiet photospheric network Variability of the quiet photospheric network

Aug 1984

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984soph...94...33m&link_type=abstract

Solar Physics (ISSN 0038-0938), vol. 94, Aug. 1984, p. 33-47.

Physics

75

Faculae, Photosphere, Solar Cycles, Solar Magnetic Field, Astronomical Photography, Field Strength, Magnetic Flux, Sunspot Cycle

Scientific paper

High-resolution photographs of the photospheric network taken in the Ca II K 3933 Å line and at λ4308 Å are analysed in order to study the variation, in latitude and over the sunspot cycle, of its density (the density is defined as the number of network elements - also called facular points - per surface unity). It appears that the density is not distributed uniformly at the surface. The density at the equator is varying in antiphase to the sunspot number. Density variations of the photospheric network express in fact variations of the quiet Sun magnetic flux. It thus results that the quiet Sun magnetic flux probably varies in antiphase to the flux in active regions. Finally, the variation over the solar cycle and the latitude distribution of photospheric network density are compared to those of X-ray bright points and ephemeral active regions.

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