Astronomy and Astrophysics – Astrophysics
Scientific paper
Sep 2006
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006aipc..858..291l&link_type=abstract
PHYSICS OF THE INNER HELIOSHEATH: Voyager Observations, Theory, and Future Prospects; 5th Annual IGPP International Astrophysics
Astronomy and Astrophysics
Astrophysics
2
Solar Wind Plasma, Sources Of Solar Wind, Heliopause And Solar Wind Termination, Planetary Bow Shocks, Interplanetary Shocks
Scientific paper
This overview talk focuses on the populations of particles which are transmitted through the nearly perpendicular termination shock from the solar wind to the heliosheath, and how they relax and excite waves in the heliosheath. The transmission process probably involves direct transmission of the very cold solar wind core. Since the shock Mach number is supercritical, an electrostatic field should form in the shock layer, causing a fraction of the incoming interstellar pickup ions to reflect. These are energized by their motion parallel to the motional electric field. Some are transmitted on the second shock encounter; others reflect many times in a shock ``surfing'' or ``skipping'' process, and gain more energy. In addition, the ``termination shock particles'' (TSPs) and the anomalous cosmic ray component (ACRs) are heated or accelerated at the shock. The distributions and pressures of all these components are estimated. The reflected pickup ions form rings or torii (with a higher-speed tail due to the multiply-reflected ions) with T⊥ > T∥. These distributions are unstable to the excitation of ion-cyclotron/Alfven waves as at Earth's bow shock; this process is described in detail. Excited wave amplitudes are estimated. Mirror-mode excitation is also investigated.
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