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The Chemical Composition of Interstellar Matter at the Solar Location

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Abstract

The Local Interstellar Cloud (LIC) surrounds the Solar System and sets the boundary conditions for the heliosphere. Using both in situ and absorption line data towards ε CMa we are able to constrain both the ionization and the gas phase abundances of the LIC gas at the Solar Location. We find that the abundances are consistent with all of the carbonaceous dust grains having been destroyed, and in fact with a supersolar abundance of C. The constituents of silicate grains, Si, Mg, and Fe, appear to be sub-solar, indicating that silicate dust is present in the LIC. N, O and S are close to the solar values.

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Authors and Affiliations

  1. Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, MS 83, Cambridge, MA, 02138, USA

    Jonathan D. Slavin

  2. Department of Astronomy & Astrophysics, University of Chicago, 5460 South Ellis Avenue, Chicago, IL, 60637, USA

    Priscilla C. Frisch

Authors
  1. Jonathan D. Slavin
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  2. Priscilla C. Frisch
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Correspondence to Jonathan D. Slavin.

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Slavin, J.D., Frisch, P.C. The Chemical Composition of Interstellar Matter at the Solar Location. Space Sci Rev 130, 409–414 (2007). https://doi.org/10.1007/s11214-007-9186-2

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  • DOI: https://doi.org/10.1007/s11214-007-9186-2

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