The physics of the heliospheric interface and its implications for LISM diagnostics

Details The physics of the heliospheric interface and its implications for LISM diagnostics The physics of the heliospheric interface and its implications for LISM diagnostics

Oct 1984

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984a%26a...139..551f&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 139, no. 2, Oct. 1984, p. 551-554.

Astronomy and Astrophysics

Astrophysics

61

Abundance, Gas-Ion Interactions, Heliosphere, Interstellar Extinction, Interstellar Gas, Space Plasmas, Charge Exchange, Hydrogen Atoms, Lyman Alpha Radiation, Neutral Gases, Resonance Fluorescence, Solar Wind, Ultraviolet Spectra

Scientific paper

The effect of the plasma interface ahead of the heliosphere on neutral interstellar gases travering this region of a perturbed interstellar plasma flow has recently been subject to some discussion. It is therefore considered necessary to briefly review the intentions and the conclusions of earlier work concerning this effect (Ripken and Fahr, 1983) and then to present some new results concerning (1) the specific extinctions of hydrogen, helium, and oxygen atoms in the interface region and (2) the interface-dependent interpretation of the Ly-alpha resonance glow data. A correct modelling of the interface effects is an indispensable prerequisite for reliable derivations of interstellar gas properties from heliospheric observations of UV/EUV resonance luminescence patterns. To achieve this an appropriate consideration of both charge exchange production and loss processes is absolutely necessary. Models invoking only loss processes or using the concept of a forward scattering probability are inadequate.

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