How conditions on the Sun affect the global heliospheric picture

Details How conditions on the Sun affect the global heliospheric picture How conditions on the Sun affect the global heliospheric picture

Dec 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011agufmsh21c..03a&link_type=abstract

American Geophysical Union, Fall Meeting 2011, abstract #SH21C-03

Astronomy and Astrophysics

Astrophysics

[2109] Interplanetary Physics / Discontinuities, [2124] Interplanetary Physics / Heliopause And Solar Wind Termination, [2126] Interplanetary Physics / Heliosphere/Interstellar Medium Interactions, [7514] Solar Physics, Astrophysics, And Astronomy / Energetic Particles

Scientific paper

The global distribution of the Sun's photopheric magnetic field directly controls the 3D structure of the corona and thus heliosphere. As the Sun's surface field evolves over the solar cycle, so does the global structure of the coronal field. During solar minimum large polar coronal holes typically dominate as the major sources of the solar wind and magnetic flux with mid-latitude/equatorial holes playing a lesser role. While during solar maximum, the polar coronal holes shrink and even briefly disappear for a time, resulting in the mid-latitude/equatorial holes playing a more dominate role. As the last solar minimum has shown, with its unusually long duration and relatively weak polar fields (i.e., compared to that of the previous two solar cycles), the time dependent evolution of the global photospheric field distribution over a given solar cycle can quantitatively differ from that of other cycles resulting in key differences in the corresponding global coronal/heliospheric configurations. In this talk, the observed photospheric magnetic field distribution over the last few solar cycles is used in the WSA model to highlight how the global coronal magnetic field configuration evolves over the solar cycle as well as how it can vary from cycle to cycle.

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