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tokens: has most of its high energy distribution below 10 keV, above which the cross section limits the charge-exchange rate. More specifically, from Figure 1 we can see that the multicomponent model has significantly more particles with 8–10 times the thermal speed compared to the kappa-distribution, and close to the TS where the total proton temperature is just over 1 MK this corresponds to protons in the 6–10 keV range. As expected, Case IV has significantly stronger source terms in the heliosheath, compared to the other three cases. As explained in Section 3.2 , in this case the electron temperature close to the TS is low, allowing for a PUI pressure that is enhanced compared to the other three cases in which the electron and proton pressures are assumed equal. Figure 2 (C) shows that case IV is about twice as efficient at removing energy from the plasma as case I (note the larger range on the color scale than in Figures 2 (A) and (B)). This has a dramatic effect on the size of the heliosphere, so that the heliopause for case IV is approximately the inner edge of the saturated blue region (see also Figure 5 ) where the source term ratio is in fact negative because the energy sources change sign at the heliopause. Figure 3 shows the ratio of the momentum source term magnitude to the magnitude of the momentum source term for a single Maxwellian. While the MHD code works with the momentum source term vector, the magnitude used in the Figure 3 can be thought of as indicating where the plasma is slowed down by charge-exchange. For the single kappa-distribution (Figure 3 (A)), the source term ratio is lower close to the TS, indicating less momentum transfer away from the plasma. The reasoning is similar to that discussed above for the energy transfer, and is a consequence of the energy-dependent cross section reducing the charge-exchange rate with the high energy wings of the distribution. Interestingly, as the plasma flows toward the heliotail, it eventually cools sufficiently for the wings of the distribution to participate in the charge-exchange process. At this point we can see an abrupt increase in the momentum source term that corresponds to a significant slowing of the plasma in the tail (this slowing of the heliotail flow is discussed in more detail in Section 3.4 ). In the more distant heliotail the source terms are similar (see also Figure 4 ), indicating that the flow speeds are similar in both the Maxwellian and kappa-distribution cases. Figure 4. Plasma (solid lines) and neutral bulk (dashed lines) properties along the line through the Sun and parallel to the direction the LISM flows from. Figure 3 (B) shows that momentum source for the multicomponent model (case III) is slightly lower than the Maxwellian case close to the TS, but similar elsewhere. Figure 3 (C) shows that in the region where the energy source for case IV greatly exceeds the corresponding source in the Maxwellian case (Figure 2 (C)), the momentum sources for case I and