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Isotopic Fractionation in Slow and Coronal Hole Associated Solar Wind

  • H. Kucharek (a1), B. Klecker (a1), F. M. Ipavich (a2), R. Kallenbach (a3), H. Grünwaldt (a4), M. R. Aellig (a5) and P. Bochsler (a6)...

Abstract

Data from the Mass and Charge Time-of-Flight spectrometers MTOF and CTOF on board SOHO have been accumulated for time periods in which coronal hole and non-coronal hole type plasma has been detected by using different methods in order to determine the abundance ratios of magnesium isotopes in these two different source regions of the solar wind. As indicators for the two different solar wind type plasma we have used several plasma parameters such as, the freeze-in temperatures, the Fe/O and the He/H ratio, which are known as reasonable indicators. For this study we have used the refractory element Mg which is an authentic whitness for matter in the solar nebula because temperatures of the Sun never have been high enough to change their isotopic composition by nuclear burning. In addition Mg has three isotopes with abundance ratios greater than about 10% and therefore they are easy to observe.

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References

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Aellig, M.R, et al., 1998, JGR, 103, 17215.
Bochsler, P, et al., 1997, Proc of the 8th Int. Solar Wind Conf, 199.
Bodmer, R. et al., 1996, Proc. of the Eur. Geophys. Soc., The Hague.
Geiss, J., et al., 1995, Space Sci. Rev., 72, 49.
Ipavich, F.M., et al., 1992, Solar Wind Seven, p 369.
Kallenbach, R., et al., 1997, JGR, 102, 26895.
Kallenbach, R., et al., 1998, Space Sci. Rev., 85, 357.
Kucharek, H., et al., 1998, JGR, 103, 26805.
v. Steiger, R., et al., 1995, Adv. Space Res., 15, (7)3.
Wimmer, R., et al., 1998, JGR, 103, 20621.

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Isotopic Fractionation in Slow and Coronal Hole Associated Solar Wind

  • H. Kucharek (a1), B. Klecker (a1), F. M. Ipavich (a2), R. Kallenbach (a3), H. Grünwaldt (a4), M. R. Aellig (a5) and P. Bochsler (a6)...

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