A 3-FLUID MODEL OF THE SOLAR-WIND TERMINATION SHOCK INCLUDING A CONTINUOUS PRODUCTION OF ANOMALOUS COSMIC-RAYS

We have formulated and numerically solved a set of differential equati ons describing the consistent dynamic and thermodynamic interaction of a coupled three-fluid plasma system in the region close to the solar wind termination shock. The three separate fluids are the solar wind p lasma, the pick-up ions, and the anomalous cosmic rays which we consid er as coupled in this region by electromagnetic induction forces and b y linear and nonlinear interactions with local wave turbulences. Here we treat the case of a continuous energy input into the anomalous cosm ic ray fluid connected with the local pick-up ion pressure and the sol ar wind velocity gradient. As free parameters within this concept we h ave to keep the average energy of the anomalous post-shock plasma and the total conversion efficiency of pick-up ions into anomalous cosmic ray particles. Related with these parameters solutions for the resulti ng shock structure can be obtained which are shown in terms of compres sion ratios, entropy generations, post-shock temperatures and post-sho ck pressures. It becomes evident that higher ratios of pick-up ion-ove r solar wind ion- densities shall definitely weaken the subshock and l ower the conversion efficiency, on the other hand increased energy inp ut rates into the anomalous plasma regime connected with higher conver sion efficiencies and pick-up ion fluxes shall also strengthen the sho ck modification and shall increase the total compression ratios. As we show solutions can be found both with and without an existing subshoc k.