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Abundances of hydrogen and helium isotopes in the Protosolar Cloud

Published online by Cambridge University Press:  23 April 2010

Johannes Geiss  and
George Gloeckler
Johannes Geiss
Affiliation:
International Space Science Institute, Hallerstrasse 6, CH-3012 Bern, Switzerland, email: geiss@issibern.ch
George Gloeckler
Affiliation:
Department of Atmospheric, Oceanic and Space Sciences, University of Michigan, 2455 Hayward St., Ann Arbor, MI 48109, USA email: gglo@umich.edu
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Abstract

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For our understanding of the origin and evolution of baryonic matter in the Universe, the Protosolar Cloud (PSC) is of unique importance in two ways: 1) Up to now, many of the naturally occurring nuclides have only been detected in the solar system. 2) Since the time of solar system formation, the Sun and planets have been virtually isolated from the galactic nuclear evolution, and thus the PSC is a galactic sample with a degree of evolution intermediate between the Big Bang and the present.

The abundances of the isotopes of hydrogen and helium in the Protosolar Cloud are primarily derived from composition measurements in the solar wind, the Jovian atmosphere and “planetary noble gases” in meteorites, and also from observations of density profiles inside the Sun. After applying the changes in isotopic and elemental composition resulting from processes in the solar wind, the Sun and Jupiter, PSC abundances of the four lightest stable nuclides are given.

Keywords

Sun: solar windcoronaabundances
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 5 , Symposium S268: Light Elements in the Universe , November 2009 , pp. 71 - 79
Copyright
Copyright © International Astronomical Union 2010

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