Magnesium isotopic abundance in slow and coronal hole associated solar wind: SOHO/CELIAS/MTOF measurements

Authors: H. Kucharek, F. M. Ipavich, R. Kallenbach, B. Klecker, H. Gruenwaldt, M. R. Aellig, P. Bochsler
Reference: Spring AGU 1999 in Boston, USA

Abstract: The solar wind provides the most comprehensive source of information about solar isotopic abundance. From in situ measurements of the solar wind one obtains informations on the present-day isotopic composition of the outer convective zone of the Sun. The flow dynamic of the solar wind is determined by the magnetic topology of the flux tubes. The slow solar wind originating from closed field line regions, has a slow bulk velocity and high freeze-in temperature, and the high speed solar wind which has a low freeze-in temperature and originates from open flux tubes in coronal holes. Data from the high resolution Mass Time-of-Flight spectrometer MTOF on board SOHO have been accumulated for time periods in which coronal hole or non-coronal hole type plasma has been detected in order to determine the abundance ratios of magnesium isotopes in these two different source regions of the solar wind.

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Last Update: April 2, 1999, James Weygand