Hostname: page-component-8448b6f56d-wq2xx Total loading time: 0 Render date: 2024-04-24T21:58:39.274Z Has data issue: false hasContentIssue false
  • English
  • Français

Changes of LISM Characteristics in the Heliospheric Interface

Published online by Cambridge University Press:  12 April 2016

Hartmut W. Ripken  and
Hans J. Fahr
Hartmut W. Ripken
Affiliation:
Institut für Astrophysik, Universität Bonn, F.R. Germany
Hans J. Fahr
Affiliation:
Institut für Astrophysik, Universität Bonn, F.R. Germany

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

It is possible to deduce LISM properties from observations of interstellar neutral gases in the inner solar system. Parameters accessible by this method are the interstellar wind vector and the densities and temperatures of hydrogen and helium, implying also the deduction of the relative abundance ratios and the degree of ionization in the LISM. Direct inference from observations, for example resonance luminescence measurements of Ly-alpha and He-58.4 nm radiation, yields values appropriate only for the inner solar system, i.e. for the regions within the heliopause dominated by the solar wind plasma.

Particularly the subsonic LISM plasma interface ahead of the heliopause causes profound changes in the properties of the neutral LISM gas traversing this region. Mainly p-H charge exchange processes give rise to the destruction of primary hydrogen and the production of secondary hydrogen atoms, the net effect being a depletion of the neutral hydrogen component of the LISM by about 50%.

Details on the depletion mechanisms, the hydrogen and oxygen extinctions, and the consequences for the Ly-alpha resonance luminescence intensity interpretations are presented.

Type
Helium and Hydrogen Backscattering Results and the Very Local Interstellar Medium
Information
International Astronomical Union Colloquium , Volume 81: Local Interstellar Medium , 1984 , pp. 28 - 31
Copyright
Copyright © NASA 1984

References

Baranov, V.B.: 1981, private communication Google Scholar
Bertaux, J.L., Blamont, J.E., Tabarie, N., Kurt, W.G., Bourgin, M.C., Smirnov, A.S., and Dementeva, N.N.: 1976, Astron. Astrophys. 46, 19–22 Google Scholar
Parker, E.N.: 1963, Interplanetary Dynamical Processes, Interscience, New York Google Scholar
Petelski, E.F., Fahr, H.J., Ripken, H.W., Brenning, N., Axnäs, I.: 1980, Astron. Astrophys. 87, 20 Google Scholar
Ripken, H.W., and Fahr, H.J.: 1983, Astron. Astrophys. 122, 181 Google Scholar
Thomas, G.E.: 1978, Ann. Rev. Earth Planetary Sci. 6, 173 Google Scholar
Wallis, M.K.: 1984, Astron. Astrophys. 130, 200 Google Scholar