Astronomy and Astrophysics – Astronomy
Scientific paper
May 2002
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002aas...200.5703m&link_type=abstract
American Astronomical Society, 200th AAS Meeting, #57.03; Bulletin of the American Astronomical Society, Vol. 34, p.737
Astronomy and Astrophysics
Astronomy
4
Scientific paper
Observations of coronal holes in context with polarity boundaries marked by filaments provide new insight into the reversals of polar magnetic polarity that occur a year or two after solar cycle maxima. Time series of solar synoptic charts of these data indicate the polarity reversal commences with the appearance of coronal holes, near latitude 40 degrees, that migrate poleward behind rows of filaments that form the polar crown. The polar crowns of both hemispheres move toward the poles beginning a few months after sunspot minimum and arrive at the poles about a year after sunspot maximum. After the polar polarity reversal (measured by the reversal of the average magnetic flux), the polar crown filaments fragment and disappear. The last of the polar crown filaments persist as much as a year after the polarity reversal; then, the coronal holes equatorward of the disssolving polar crown encircle, then cover, the solar poles. These become the polar caps that will persist until the next sunspot maximum. Observations of the current solar cycle reveal a surprizing possibility that the new polar coronal holes originate at sunspot maximum from remnants of polar coronal holes in the opposite solar hemisphere. A pole-to-pole migration of coronal holes is not expected with a Babcock-Leighton-Sheeley model of the solar cycle. E-mail pmcintosh@solar.stanford.edu Telephone: 303-444-5880
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