Modulation and Demodulation

Marsch, Patrick; Penttinen, Jyrki T. J.

doi:10.1002/9781118678916.ch10

Cited by 1 publication

(1 citation statement)

References 2 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…The FIP effect is attributed to the preferential ionization of low-FIP elements in the chromosphere, which are then entrained into the solar wind via mechanisms such as ambipolar diffusion (e.g., Marsch et al 1995), inefficient Coulomb drag (Buergi & Geiss 1986;Buergi 1992;Bodmer & Bochsler 1998 or wave-particle interaction (Schwadron et al 1999;Laming 2004). The SW elemental fractionation depends on the region of the Sun from which the flow originates.…”

Section: Introductionmentioning

confidence: 99%

VARIATIONS IN SOLAR WIND FRACTIONATION AS SEEN BYACE/SWICS AND THE IMPLICATIONS FORGENESISMISSION RESULTS

Pilleri

Reisenfeld

Zurbuchen

et al. 2015

ApJ

View full text Add to dashboard Cite

We use ACE/SWICS elemental composition data to compare the variations in solar wind fractionation as measured by SWICS during the last solar maximum (1999)(2000)(2001), the solar minimum (2006)(2007)(2008)(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. 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

show abstract