Is the solar wind termination shock a cosmic-ray mediated shock?

Details Is the solar wind termination shock a cosmic-ray mediated shock? Is the solar wind termination shock a cosmic-ray mediated shock?

Dec 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005agufmsh51a1192k&link_type=abstract

American Geophysical Union, Fall Meeting 2005, abstract #SH51A-1192

Physics

2124 Heliopause And Solar Wind Termination, 2126 Heliosphere/Interstellar Medium Interactions, 7859 Transport Processes, 7863 Turbulence (4490), 7867 Wave/Particle Interactions (2483, 6984)

Scientific paper

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.

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