Cool heliosheath plasma and deceleration of the upstream solar wind at the termination shock

Details Cool heliosheath plasma and deceleration of the upstream solar wind at the termination shock Cool heliosheath plasma and deceleration of the upstream solar wind at the termination shock

Jul 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008natur.454...63r&link_type=abstract

Nature, Volume 454, Issue 7200, pp. 63-66 (2008).

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Scientific paper

The solar wind blows outward from the Sun and forms a bubble of solar material in the interstellar medium. The termination shock occurs where the solar wind changes from being supersonic (with respect to the surrounding interstellar medium) to being subsonic. The shock was crossed by Voyager 1 at a heliocentric radius of 94AU (1AU is the Earth-Sun distance) in December 2004 (refs 1-3). The Voyager 2 plasma experiment observed a decrease in solar wind speed commencing on about 9 June 2007, which culminated in several crossings of the termination shock between 30 August and 1 September 2007 (refs 4-7). Since then, Voyager 2 has remained in the heliosheath, the region of shocked solar wind. Here we report observations of plasma at and near the termination shock and in the heliosheath. The heliosphere is asymmetric, pushed inward in the Voyager 2 direction relative to the Voyager 1 direction. The termination shock is a weak, quasi-perpendicular shock that heats the thermal plasma very little. An unexpected finding is that the flow is still supersonic with respect to the thermal ions downstream of the termination shock. Most of the solar wind energy is transferred to the pickup ions or other energetic particles both upstream of and at the termination shock.

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