A 2-FLUID MODEL OF THE SOLAR-WIND TERMINATION SHOCK MODIFIED BY SHOCK-GENERATED COSMIC-RAYS INCLUDING ENERGY-LOSSES

We consider the formation of the heliospheric termination shock in a t wo-fluid approximation including the self-consistent dynamic interacti on of the thermal solar wind ion plasma and a shock-generated high ene rgy cosmic ray gas representing the so-called anomalous cosmic ray com ponent. Due to the diffusive interaction of the two media an extended structure of the shock is formed consisting of a precursor region and a gas dynamic sub-shock. Pick-up ions, convected with the thermal plas ma to the sub-shock, at a fraction eta serve there as a seed for high energy particles which by first order Fermi acceleration in the shock- induced wave turbulences are energized from KeV- to MeV-energies. Here we treat in a consistent manner the spatial diffusion of such high en ergy particles in the resulting solar wind flow structure and therefor e solve a coupled system of differential equations adequately describi ng mass-, momentum-, and energy-flow continuities for both the low and the high energy plasma component. The energy loss due to the leakage of high energy particles upstream from the shock structure is taken in to account. In the results we then can show how the shock-generated, e nergetic cosmic ray particles influence the structure of the shock. We demonstrate the variation of the compression ratio in the termination shock as function of the conversion efficiency eta and on the mean en ergy of the shock-generated cosmic ray particles. Furthermore we discu ss the influence of the energy loss due to the upstream leakage of sho ck-generated, high energy particles on the dimension of the heliosheat h plasma, i.e. on the distance between the termination shock and the h eliopause. As it turns out from our calculations the upwind heliosheat h dimension can be reduced by up to 25 percent for high conversion eff iciencies.