Solar wind composition

F. R. Wimmer-Schweingruber, O. Kern, and C. D. Hamilton. On the Solar Wind Composition During the November 1997 Solar Particle Events WIND/MASS Observations, Geophys. Res. Lett., 26, no. 23 (1999) 3541-3544. 

R. C. Wiens, D. S. Burnett, C. M. Hohenberg, A. Meshik, V. Heber, A. Grimberg, R. Wieler, and D. B. Reisenfeld. Solar and Solar-Wind Composition Results from the Genesis Mission, Space Science Reviews, 130, no. 1-4(2007) 161-171. 

Figure 7. A few examples of isotopic patterns of Ne, Ti and heavy elements in SiC and graphite grains are displayed. Absolute ratios are plotted for Ne (a) whereas abundance ratios relative to solar wind composition are plotted for Kr (c) and Xe (f). The remaining elements are plotted as %o deviations from laboratory standards. The data have been obtained on bulk SiC separates by traditional mass spectrometry for Ne (Jungck and Eberhardt 1979), Kr (Ott et al. 1988 Lewis et al. 1994), Sr, Ba (Ott and Begemann 1990 Prombo et al. 1993) and Nd (Richter 1995). SIMS techniques (caption continued on facing page)...

Figure 2.15 Ne three-isotope plot for a grain-size suite of plagioclase separates from lunar high land soil that were treated by the CSSE treatment (see text). The best fitted line through the data from all etched samples (line p) passes close to the data point GCR (galactic cosmic ray) of cosmogenic Ne. On the left side, the path of mass fractionation of SWC (solar wind composition)-Ne intersects line p at a 20Ne/22Ne ratio of -11.3, which is interpreted to represent SEP (solar energetic particle) Ne (cf. Section 2.8). Open symbols unetched sample. Solid symbols etched samples. SF Solar flare Ne. Reproduced from Signer et al. (1993).

Table 3.1) concentration. The ordinate position of the solar wind composition is arbitrary. The vertical dashed lines illustrate roughly the magnitude of typical in situ contributions at He, the horizontal tick is for 4He, whereas the upward extension is for 3He trapped gases at lower concentrations would be difficult to identify. Solar wind composition from Table 3.2, lunar ilmenites from Eberhardt et al., 1972 and Pesyanoe from Marti, 1969. All the patterns shown here are of the solar type (cf. Figure 3.2 for the planetary type). 

Geiss, J., Buehler, F., Cerutti, H., Eberhardt, P., Filleaux, C. H. (1972) Solar wind composition experiments. Apollo 15 Preliminary Scientific Report, NASA SP-289, pp. 15-1-15-7. 

Nichols, R. H., Jr., Hohenberg, C. M., Olinger, C. T. (1994) Implanted solar helium, neon, and argon in individual lunar ilmenite grains Surface effects and temporal variation in the solar wind composition. Geochim. Cosmochim. Acta, 58, 1031-42. 

Geiss J., Gloeckler G., and von Steiger R. (1994) Solar and heliospheric processes from solar wind composition measurements. Phil. Trans. Roy. Soc. London A 349, 213-226. 

The Kr and Xe isotopic compositions in the solar wind have not yet been determined directly, neither in space nor with foils. On the other hand, lunar soil samples are well suited to study the isotopic composition of these elements in the solar wind, because the moon contains hardly any indigenous Kr and Xe. The good agreement of the He and Ne compositions deduced from regolithic samples with the values determined in situ or the Apollo solar wind composition experiment gives us confidence that the lunar data for the two heavy noble gases are also reliable. Frequently used recent values are given in Table... 

BochslerP (1994) Solar wind composition from the moon. Adv Space Res 14 161-173 Bochsler P (2000) Abundances and charge states of particles in the solar wind. Rev Geophys 38 247-266 Bochsler P, Geiss J, Maeder A (1990) The abundance of He in the solar wind—a constraint for models of solar evolution. Solar Phys 128 203-215... 

Geiss J (1973) Solar wind composition and implications about the history of the solar system. Conf Paper 13th Inti Cosmic Ray Conf 3375-3398... 

Geiss J, Btihler F, Cerutti H, Eberhardt P, Filleux C (1972) Solar wind composition experiment. Apollo 16 Prelim Sci Rep, NASA SP-315 14.11-14.10... 

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