Solar cycle variation of ephemeral active regions

Details Solar cycle variation of ephemeral active regions Solar cycle variation of ephemeral active regions

Nov 1984

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984esasp.220..235h&link_type=abstract

In ESA The Hydromagnetics of the Sun p 235-236 (SEE N85-25091 14-92)

Physics

15

Photosphere, Solar Cycles, Sunspots, Magnetic Flux, Magnetic Signatures, Solar Activity Effects, Solar Flux, Solar Magnetic Field

Scientific paper

Ephemeral active regions (ER) were identified and counted for periods from 1970 to mid-1984 using daily, full-disk photospheric magnetograms. The number of ER varies in phase with the solar cycle. At solar minimum, ER are distributed almost uniformly in latitude; by solar maximum, peaks in the latitude distribution are observed in the sunspot zones and in two higher bands. From 20% to 30% of the He I 10830 dark points, used as a proxy for X-ray bright points (XBP), are associated with ER; 70% to 80% overlie bipoles that appear to be the chance encounter of opposite polarity network. It is suggested that ER are primarily surface phenomena, resulting from convection interacting with subphotospheric fields; and XBP are associated with the chance encounter of network flux, the occurrence of which is related to the amount of mixed polarity areas which varies inversely with the solar cycle.

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