Astronomy and Astrophysics – Astrophysics
Scientific paper
Dec 2009
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009agufmsh14a..04a&link_type=abstract
American Geophysical Union, Fall Meeting 2009, abstract #SH14A-04
Astronomy and Astrophysics
Astrophysics
[7509] Solar Physics, Astrophysics, And Astronomy / Corona, [7524] Solar Physics, Astrophysics, And Astronomy / Magnetic Fields, [7536] Solar Physics, Astrophysics, And Astronomy / Solar Activity Cycle
Scientific paper
Altrock (1997, Solar Phys. 170, 411) 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 emission 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 emission 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 emission appeared near 70 degrees latitude and began migrating towards the equator, but at a rate 40% slower than the previous two solar cycles. However, the onset of the "Rush to the Poles" of polar crown prominences and their associated coronal emission, which has preceded solar maximum by approximately two years in recent cycles (cf. Altrock, 2003, Solar Phys. 216, 343), has just occurred. Implications of these two events for predictions of the timing of the maximum of cycle 24 will be discussed. The observations used herein are the result of a cooperative program of the Air Force Research Laboratory and the National Solar Observatory.
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