The Importance of Non-Thermal Pressures in the Heliosheath: Towards New Methods of Analysis

The in-situ plasma measurements when Voyager 2 crossed the termination shock into the heliosheath revealed that only ~20% of the downstream pressure resided in the thermal ion population at energies << 1 keV. The LECP ion measurements > 30 keV at both VGRs 1 and 2 implied a partial pressure ΔP~0.02pPa that accounted for another ~15% of the total pressure. Adding in the missing 70% of the non-thermal pressure, the total non-thermal pressure at the VGRs must be P~0.12pPa. Consensus estimates of the local interstellar magnetic field (ISMF) are near B~0.25nT which gives a hydrostatic magnetic pressure B2/2μ0~0.25pPa. Cassini/INCA all-sky images of 5-44keV ENAs from the heliosheath [Krimigis et al., this session] show that neither VGR1 nor VGR2 is in the direction of maximum ENA emission. Consequently, it is possible that the pressure of non-thermal protons in the heliosheath is comparable to the hydrostatic pressure of the interstellar magnetic field (ISMF) that confines the heliosheath. An immediate corollary is that we will not understand the physics of the heliosheath until we find ways of quantitatively describing the dynamics of pressures produced by non-thermal ion populations. Present MHD theories and simulations simply do not capture these essential dynamical processes. We point out that the magnetospheric communities studying the dynamics of non-thermal ion injections (with plasma beta>1) at Earth and Saturn revealed by ENA imaging have been making significant progress in a quite similar problem. We offer some possible approaches for the quantitative analysis of the heliosheath, based on the magnetospheric experience.