The Progress of Solar Cycle 24 at High Latitudes

Details The Progress of Solar Cycle 24 at High Latitudes The Progress of Solar Cycle 24 at High Latitudes

May 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009spd....40.2405a&link_type=abstract

American Astronomical Society, SPD meeting #40, #24.05; Bulletin of the American Astronomical Society, Vol. 41, p.861

Astronomy and Astrophysics

Astronomy

Scientific paper

Altrock (Solar Phys., 170, 411, 1997) and earlier authors discussed the high-latitude "extended" solar cycle seen in the Fe XIV corona prior to the appearance of sunspots and active regions at lower latitudes. For example, persistent coronal activity appeared near 70 degrees latitude in 1979 and 1989 and slowly migrated towards the equator, merging with the latitudes of sunspots and active regions after several years. Altrock (2007AGUFMSH53A1052A) showed that the high-latitude coronal activity was situated above the high-latitude neutral line of the large-scale photospheric magnetic field seen in Wilcox Solar Observatory synoptic maps, thus implying a connection with the solar dynamo.
In 1999, persistent Fe XIV coronal activity appeared near 70 degrees latitude and began slowly migrating towards the equator at a rate similar to the previous two solar cycles. Thus, it appears that the solar dynamo that will produce the activity of cycle 24 is progressing normally. The current state of the extended solar cycle will be presented, with emphasis on determining whether the "Rush to the Poles" that will herald the cycle 24 maximum has begun (cf. Altrock, Solar Phys., 216, 343, 2003). Samples of current solar-minimum coronal activity will be shown.

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