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Newly synthesized lithium in the interstellar medium

Nature volume 405, pages 656658 (08 June 2000) | Download Citation

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Abstract

Astronomical observations of elemental and isotopic abundances provide the means to determine the source of elements and to reveal their evolutionary pathways since the formation of the Galaxy some 15 billion years ago. The abundance of lithium is particularly interesting because, although some of it is thought to be primordial, most results from spallation reactions (in which Galactic cosmic rays break apart larger nuclei in the interstellar medium). Spallation reactions are crucial for the production of other light elements1, such as beryllium and boron, so observations of lithium isotopic abundances can be used to test model predictions2,3,4,5 for light-element synthesis in general. Here we report observations of 7Li and 6Li abundances in several interstellar clouds lying in the direction of the star ο Persei. We find the abundance ratio 7Li/6Li to be about 2, which is significantly lower than the average Solar System value of 12.3 (refs 6, 7). An abundance ratio of 2 is clear evidence that the observed lithium must have resulted entirely from spallation, confirming a basic tenet of light-element synthesis2,3,4,5. The total lithium abundance, however, is not enhanced as expected.

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Acknowledgements

We thank E. Parizot and H. Reeves for fruitful discussions. This work was supported by the National Aeronautics and Space Administration. We made use of the Simbad database, operated at Centre de Donées Astronomiques de Strasbourg, Strasbourg, France.

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  1. *Department of Physics & Astronomy, University of Toledo, Toledo, Ohio 43606, USA

    • D. C. Knauth
    •  & S. R. Federman
  2. †Department of Astronomy, University of Texas, Austin, Texas 78712, USA

    • David L. Lambert
  3. ‡Department of Physics & Astronomy, Dartmouth College, Hanover, New Hampshire 03755, USA, and NASA Headquarters, Washington DC, 20546, USA

    • P. Crane

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Correspondence to S. R. Federman.

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https://doi.org/10.1038/35015028

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