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Isotopic Fractionation in Slow and Coronal Hole Associated Solar Wind

Published online by Cambridge University Press:  13 May 2016

H. Kucharek ,
B. Klecker ,
F. M. Ipavich ,
R. Kallenbach ,
H. Grünwaldt ,
M. R. Aellig  and
P. Bochsler
H. Kucharek
Affiliation:
Max-Planck-Institut für extraterrestrische Physik, P.O. Box 1312, 85741 Garching, Germany
B. Klecker
Affiliation:
Max-Planck-Institut für extraterrestrische Physik, P.O. Box 1312, 85741 Garching, Germany
F. M. Ipavich
Affiliation:
University of Maryland, College Park, USA
R. Kallenbach
Affiliation:
International Space Science Institute, Bern, Switzerland
H. Grünwaldt
Affiliation:
Max-Planck-Institut für Aeronomie, Katlenburg-Lindau, Germany
M. R. Aellig
Affiliation:
MIT/Center for Space Research, Cambridge, USA
P. Bochsler
Affiliation:
Physikalisches Institut, Universität Bern, Bern, Switzerland

Abstract

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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.

Type
Session VI: The Solar Wind and Heliosphere
Information
Symposium - International Astronomical Union , Volume 203: Recent Insights into the Physics of the Sun and Heliosphere: Highlights from Soho and Other Space Missions , 2001 , pp. 562 - 564
Copyright
Copyright © Astronomical Society of the Pacific 2001 

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