The Multifluid Character of the `Baranov' Interface |
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Authors: | HJ Fahr |
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Institution: | 1. Institut für Astrophysik und Extraterrestrische Forschung der, Universit?t Bonn, Auf dem Hügel 71, D–53121, Bonn, Germany; E-mail
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Abstract: | Since about three decades now it is clearly recognized that the interaction of the solar system with the ambient interstellar
medium flow mainly is characterized by its hydrodynamic nature invoking structures like the inner shock, the heliopause and
the outer shock with plasma sheath regions in between. After the pioneering works by Eugene Parker and Vladimir Baranov the
main outlines of this interaction scenario were established, while some discussion on location and geometry of these structures
is still going on till now. Fundamentally new aspects of this interaction problem have meanwhile appeared calling for new
and more consistent calculations. The revisions of the earlier interaction concept starts with the neutral LISM gas component
passing through the solar system. At the occasion of ionizations of this component a medium-energetic plasma component in
form of keV-energetic pick-up ions is created. This component changes the distant solar wind properties by mass-, momentum-,
and energy-loading, by wave generation and lowering the solar wind Mach numbers. Furthermore pick-up ions serve as a seed
population for a high-energetic plasma population with energies between 10 and 100 MeV/nuc called anomalous cosmic rays. This
latter component by means of its pressure gradient not only modifies the solar wind flow but also modulates its termination
shock. In this paper it is shown how the main features of the enlarged interaction scenario change if the above mentioned
multifluid character of the scenario is taken into account. While now we present a `multicolour vision' of the interacting
heliosphere, it should never be forgotten that these modern views only were possible due to the fundamental `black-and-white
vision' already presented by Baranov in the seventieths.
This revised version was published online in July 2006 with corrections to the Cover Date. |
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