Observations of the High-Latitude Interplanetary Helium Abundance with Ulysses

Details Observations of the High-Latitude Interplanetary Helium Abundance with Ulysses Observations of the High-Latitude Interplanetary Helium Abundance with Ulysses

Dec 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006agufmsh23b0362s&link_type=abstract

American Geophysical Union, Fall Meeting 2006, abstract #SH23B-0362

Physics

7509 Corona, 7536 Solar Activity Cycle (2162), 7845 Particle Acceleration

Scientific paper

We have previously reported trends in the variations in the solar wind helium abundance as a function of bulk speed and heliographic latitude using the Wind spacecraft. The relative abundance by number density of helium to hydrogen (He/H) near the heliographic equator is a clear function of latitude at solar minimum. While it has been suggested that low He/H near the ecliptic is the signature of the heliospheric current sheet (HCS), we have shown that the relationship extends beyond the HCS signature. We present an extension of this study into higher latitudes and the predominantly fast solar wind using the Ulysses fast latitude scan. We demonstrate that the latitude dependence of He/H extends beyond the narrow range explored by the Wind spacecraft in Earth orbit. We also demonstrate an inverse correlation between He/H and the differential flow speed between hydrogen and helium. We suggest that latitudinal He/H variation may be interpreted as a tracer for the latitudinal gradient in the strength of the wave-resonant processes associated with differential flow in the solar minimum corona.

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