Structure of the Heliospheric Termination Shock

Details Structure of the Heliospheric Termination Shock Structure of the Heliospheric Termination Shock

Dec 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008agufmsh14a..03z&link_type=abstract

American Geophysical Union, Fall Meeting 2008, abstract #SH14A-03

Physics

2124 Heliopause And Solar Wind Termination, 4455 Nonlinear Waves, Shock Waves, Solitons (0689, 2487, 3280, 3285, 4275, 6934, 7851, 7852)

Scientific paper

Observations by the Voyager 2 spacecraft of the structure of the heliospheric termination shock revealed a quasi-perpendicular structure that possessed many of the characteristics that are familiar to us from perpendicular shocks observed in the inner heliosphere. Because the Voyager plasma instrument cannot measure the interstellar pickup ions directly, their behavior at the termination shock could not be gauged. Nonetheless, it had already been predicted by Zank et al. 1996 that the primary dissipation mechanism for the quasi-perpendicular termination shock would be the reflection of pickup ions rather than solar wind ions; this because of the shell-like structure of the pickup ion distribution function. We discuss the interaction of pickup ions through their trajectories within the structure of the shock observed by Voyager 2. A model for the shock structure is constructed on the basis of preferentially reflected pickup ions, and solutions are presented.

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