Flux Transport and the Sun's Polar Magnetic Fields at Cycle 23/24 Minimum

Details Flux Transport and the Sun's Polar Magnetic Fields at Cycle 23/24 Minimum Flux Transport and the Sun's Polar Magnetic Fields at Cycle 23/24 Minimum

Dec 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011agufmsh23d..02u&link_type=abstract

American Geophysical Union, Fall Meeting 2011, abstract #SH23D-02

Astronomy and Astrophysics

Astrophysics

[7524] Solar Physics, Astrophysics, And Astronomy / Magnetic Fields, [7536] Solar Physics, Astrophysics, And Astronomy / Solar Activity Cycle

Scientific paper

The polar magnetic fields observed on the Sun during the Cycle 23/24 minimum were substantially weaker than those observed for the previous three minima. In most dynamo models weak polar fields result in weak following cycles, which are observed to start late and leave behind a long low minimum. While this accounts for the peculiarities observed during the Cycle 23/24 minimum, it begs an explanation for why the polar magnetic fields were so weak. Here we model the transport of magnetic flux from active region sources via the observed magnetic element differential rotation and meridional flow from 1996 to 2011 (Hathaway & Rightmire ApJ 729:80, 2011). The active region sources are characterized by the observed sizes and locations of the leading and following polarity magnetic flux. Both the sources of the flux and the flows that transport them are fully constrained by observations. Comparisons will be made between the observed and modeled polar field reversals and the final polar field strengths. Conclusions will be drawn concerning the need for additional flux transport processes.

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