May 2004
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004aps..nws.c1004s&link_type=abstract
American Physical Society, Northwest Section Spring 2004 Meeting, 21-22 May, 2004, Pullman, WA. MEETING ID: NWS04, abstract #C1
Physics
Scientific paper
How is the solar dynamo related to sunspots? Sunspots are easy to observe as they appear on the surface of the sun. George Hale demonstrated that where there are sunspots there is also a strong magnetic field projecting through the photosphere. It is assumed that a dynamo at the base of the convection zone generates the magnetic flux we observe on the surface of the sun. As we cannot directly observe the magnetic fields underneath the photosphere, we use the sunspot and magnetic pole reversal cycles to model the dynamo. The Babcock-Leighton dynamo model describes the main features of the solar cycle through differential rotation and the convection process, but does not account for many of the details, and is inconsistent with observations of internal solar flows from helioseismology. Mausumi Dikpati and colleagues are developing a dynamo model that incorporates the circulation of plasma from the equator to the poles, called the meridional flow. Magnetic field lines are "frozen" into this plasma, recording part of the previous polar cycle in the meridional flow, which could then become the seed for a regenerating field. I hope to analyze the meridional flow data from the previous two to three cycles in order to understand the unusual sunspot features in the current cycle and to predict future cycles. References: Dikpati, M., et al. Diagnostics of polar field reversal in solar cycle 23 using a flux transport dynamo model, 2004, ApJ 601.
Song Night
Zita E. J.
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