The multifluid character of the 'Baranov' interface

Since about three decades now it is clearly recognized that the interaction of the solar system with the ambient interstellar medium flow mainly is ch aracterized by its hydrodynamic nature invoking structures like the inner s hock, the heliopause and the outer shock with plasma sheath regions in betw een. After the pioneering works by Eugene Parker and Vladimir Baranov the m ain outlines of this interaction scenario were established, while some disc ussion on location and geometry of these structures is still going on till now. Fundamentally new aspects of this interaction problem have meanwhile a ppeared 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 co mponent a medium-energetic plasma component in form of keV-energetic pick-u p ions is created. This component changes the distant solar wind properties by mass-, momentum-, and energy-loading, by wave generation and lowering t he solar wind Mach numbers. Furthermore pick-up ions serve as a seed popula tion for a high-energetic plasma population with energies between 10 and 10 0 MeV/nuc called anomalous cosmic rays. This latter component by means of i ts pressure gradient not only modifies the solar wind flow but also modulat es its termination shock. In this paper it is shown how the main features o f the enlarged interaction scenario change if the above mentioned multiflui d character of the scenario is taken into account. While now we present a ' multicolour vision' of the interacting heliosphere, it should never be forg otten that these modern views only were possible due to the fundamental 'bl ack-and-white vision' already presented by Baranov in the seventieths.