HR: 0800h
AN: SH51A-1192    [Abstracts]
TI: Is the solar wind termination shock a cosmic-ray mediated shock?
AU: * Kallenbach, R
EM: kallenbach@issi.unibe.ch
AF: International Space Science Institute, Hallerstrasse 6, Bern, BE 3012 Switzerland
AU: Izmodenov, V
EM: izmod@ipmnet.ru
AF: Lomonosow Moscow State University, School of Mechanics and Mathematics, Department of Aeromechanics and Gas Dynamics, GSP-2, Leninskie Gory, Moscow, 119899 Russian Federation
AB: Recent data from Voyager 1 crossing the solar wind termination shock into the inner heliosheath and data on energetic neutral atoms detected by SOHO/CELIAS/HSTOF constrain the diffusion parameters and therefore the level of magnetic fluctuations which are relevant for the acceleration and transport of Anomalous Cosmic Rays (ACRs) or Termination Shock Energetic Particles (TSEPs). We compare the data to a model on the evolution of solar wind turbulence with heliocentric distance. This model includes turbulence amplified by 1) stream-stream interactions, 2) pick-up ions 3) TSEPs and ACRs, and 4) the termination shock itself. The injection efficiencies of several species of ACRs and TSEPs and their back reaction on the termination shock are calculated in a self-consistent manner and compared to the data. In particular, the influence of ACRs (TSEPs) on the location of the solar wind termination shock is discussed in the frame of a global time-dependent multi-component model of the solar wind interaction with the local interstellar medium. This model takes into account the mutual influence of solar wind protons, electrons, pickup ions, ACRs, and magnetic fields.
DE: 2124 Heliopause and solar wind termination
DE: 2126 Heliosphere/interstellar medium interactions
DE: 7859 Transport processes
DE: 7863 Turbulence (4490)
DE: 7867 Wave/particle interactions (2483, 6984)
SC: SPA-Solar and Heliospheric Physics [SH]
MN: Fall Meeting 2005