Structure and properties of the termination shock

Details Structure and properties of the termination shock Structure and properties of the termination shock

Sep 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004aipc..719..329z&link_type=abstract

PHYSICS OF THE OUTER HELIOSPHERE. AIP Conference Proceedings, Volume 719, pp. 329-340 (2004).

Physics

2

Particle Emission, Solar Wind, Solar Wind Plasma, Sources Of Solar Wind, Planetary Bow Shocks, Interplanetary Shocks

Scientific paper

Conventionally, the heliospheric termination shock (HTS) is regarded as a sharp MHD discontinuity. More recent models suggest that the back-reaction of energetic cosmic rays accelerated at the HTS will create a broad shock with an extended precursor. Here we suggest that a combination of upstream solar wind disturbances interacting with the HTS, the presence of cosmic ray gradient-driven instabilities and their coupling to the pickup ion population yields a termination shock that is highly dynamical in both structure and location. We also suggest that the diffusive cosmic ray transport equation used to model particle acceleration at a shock may require modification to account for a highly turbulent velocity component.

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