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3He and4He in the local interstellar gas as observed with the COLLISA foil experiment on the Mir space station

Published online by Cambridge University Press:  23 December 2005

P. Bochsler ,
Yu. N. Agafonov ,
F. Bühler ,
H. Busemann ,
N. A. Eismont ,
A. Grimberg ,
V. S. Heber ,
E. Salerno ,
R. Wieler  and
G. N. Zastenker
P. Bochsler
Affiliation:
Physikalisches Institut, University of Bern, Sidlerstrasse 5, CH-3012 Bern, Switzerland email: [email protected]
Yu. N. Agafonov
Affiliation:
Space Research Institute (IKI), Russian Academy of Sciences, Moscow, Russia
F. Bühler
Affiliation:
Physikalisches Institut, University of Bern, Sidlerstrasse 5, CH-3012 Bern, Switzerland email: [email protected]
H. Busemann
Affiliation:
Physikalisches Institut, University of Bern, Sidlerstrasse 5, CH-3012 Bern, Switzerland email: [email protected] Present address: Department of Terrestrial Magnetism, Carnegie Institution of Washington, Washington D.C., USA
N. A. Eismont
Affiliation:
Space Research Institute (IKI), Russian Academy of Sciences, Moscow, Russia
A. Grimberg
Affiliation:
Institut für Isotopengeologie und Mineralische Rohstoffe, ETH Zürich, Switzerland
V. S. Heber
Affiliation:
Institut für Isotopengeologie und Mineralische Rohstoffe, ETH Zürich, Switzerland
E. Salerno
Affiliation:
Physikalisches Institut, University of Bern, Sidlerstrasse 5, CH-3012 Bern, Switzerland email: [email protected]
R. Wieler
Affiliation:
Institut für Isotopengeologie und Mineralische Rohstoffe, ETH Zürich, Switzerland
G. N. Zastenker
Affiliation:
Space Research Institute (IKI), Russian Academy of Sciences, Moscow, Russia
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Abstract

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With the COLLISA foil experiment onboard the Mir space station we have collected samples of interstellar helium, which have been returned to the Earth and investigated by mass spectrometric analysis. Recently, we have been able to reduce the experimental uncertainties as given earlier (Salerno et al. 2003). Our improved estimate of the helium isotopic ratio in the local interstellar medium is now ($^3$He/$^4$He)$_{LISM}$=(1.62 $\pm$ 0.29)$\,{\times}\,$10$^{-4}$ (Busemann et al. 2005).

Keywords

ISM: abundancesGalaxy: abundancesGalaxy: evolution
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 1 , Symposium S228: From Lithium to Uranium: Elemental Tracers of Early Cosmic Evolution , May 2005 , pp. 77 - 80
Copyright
© 2005 International Astronomical Union