Source Regions of Helium Variations in the Slow Solar Wind

Details Source Regions of Helium Variations in the Slow Solar Wind Source Regions of Helium Variations in the Slow Solar Wind

Dec 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008agufmsh43b..04m&link_type=abstract

American Geophysical Union, Fall Meeting 2008, abstract #SH43B-04

Physics

7509 Corona, 7511 Coronal Holes, 7924 Forecasting (2722), 7959 Models

Scientific paper

The relative abundances of helium and hydrogen in the solar wind vary on solar cycle time scales as well as with solar wind speed. Kasper et al., 2007 demonstrated further that, during solar minimum, the relative helium abundance correlated with the heliographic latitude of the observer. They also found a linear relationship between the solar wind speed and relative helium abundance for slow (less than 550 km/s) solar wind. Mapping the in situ measurements back to the solar wind source region allows us to relate helium abundance to conditions at the sun. We investigate the coronal sources of the relative helium abundance variations using the WSA-ENLIL model. Improvements to the WSA-ENLIL model have led to better solar wind predictions. Using these improved simulations of the connection between the corona and interplanetary space, we determine the source regions for several time periods during solar minimum when the predicted solar wind speed yields good results as compared with observations. We investigate helium abundance as a function of source region properties such as distance to the current sheet, magnetic expansion factor and the distance to the edge of a coronal hole.

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