The Sun's Magnetic Field During The Past Two Minima

Details The Sun's Magnetic Field During The Past Two Minima The Sun's Magnetic Field During The Past Two Minima

May 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009spd....40.1110d&link_type=abstract

American Astronomical Society, SPD meeting #40, #11.10; Bulletin of the American Astronomical Society, Vol. 41, p.827

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The past three years have been characterized by a very weak sunspot and CME activity making this a long and deep solar minimum. In spite of the lack of magnetic activity at the Sun, white light and EUV images have shown that a dimmer but relatively complex corona -with multiple streamers and low latitude coronal holes- persisted during most of this extended minimum. Solar wind observations indicated an increase in solar wind velocity near the Earth and a more warped heliopsheric current sheet during the declining and minimum phase of this cycle. Interestingly, the polar magnetic fields observed at the photosphere during the present minimum are 30-40% weaker than during the previous minimum.
Can the weaker polar fields (and associated weaker dipole moment) explain the differences observed in the corona and heliosphere? To answer this question, we will use PFSS model computations. We will run the Wang-Sheeley-Arge model from 1996 to the present to determine the relative importance of the dipole moment vs. higher moments during the two minimum periods. We will then artificially modify the polar magnetic field strength during the two minima to investigate how increasing/decreasing the strength of the polar fields during the present/past minimum changes the derived coronal holes and coronal field.

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