Variations in Solar Wind Fractionation as Seen by ACE/SWICS Over a Full Solar Cycle and the Implications for Genesis Mission Results

Tuesday, 15 December 2015: 11:35
2009 (Moscone West)
Daniel Brett Reisenfeld1, Paolo Pilleri2, Thomas Zurbuchen3, Susan T Lepri4, Paul Shearer3, Jason A Gilbert3, Rudolf von Steiger5 and Roger C Wiens6, (1)University of Montana, Department of Physics & Astronomy, Missoula, MT, United States, (2)University Paul Sabatier Toulouse III, Toulouse Cedex 09, France, (3)University of Michigan Ann Arbor, Ann Arbor, MI, United States, (4)Univ Michigan, Ann Arbor, MI, United States, (5)International Space Science Institute, Bern, Switzerland, (6)Space Science and Applications, Los Alamos, NM, United States
We use ACE/SWICS elemental composition data to compare the variations in solar wind fractionation as measured by SWICS during the previous solar maximum (1999-2001), solar minimum (2006-2009) and the period in which the Genesis spacecraft was collecting solar wind (late 2001 - early 2004). We differentiate our analysis in terms of solar wind regimes (i.e. solar wind originating from interstream or coronal hole flows, or coronal mass ejecta). Abundances are normalized to the low-FIP ion magnesium to uncover correlations that are not apparent when normalizing to high-FIP ions.

We find that relative to magnesium, the other low-FIP elements are measurably fractionated, but the degree of fractionation does not vary significantly over the solar cycle. For the high-FIP ions, variation in fractionation over the solar cycle is significant: greatest for Ne/Mg and C/Mg, less so for O/Mg, and the least for He/Mg. When abundance ratios are examined as a function of solar wind speed, we find a strong correlation, with the remarkable observation that the degree of fractionation follows a mass-dependent trend. We will discuss the implications for correcting the Genesis sample return results to photospheric abundances.