Modeling the effects of fast shocks on solar winds ions

Details Modeling the effects of fast shocks on solar winds ions Modeling the effects of fast shocks on solar winds ions

Apr 1991

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991jgr....96.5437z&link_type=abstract

Journal of Geophysical Research (ISSN 0148-0227), vol. 96, April 1, 1991, p. 5437-5445.

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13

Interplanetary Magnetic Fields, Interplanetary Medium, Ion Distribution, Plasma Composition, Shock Waves, Solar Wind, Cross Flow, International Sun Earth Explorer 3, Magnetic Field Configurations, Particle Mass

Scientific paper

Observations show that, when alpha particles and other minor ions in the solar wind plasma encounter fast shocks, they are heated more than protons and their bulk motion is decelerated less than protons. These effects have been studied using a three-fluid model, and the model predictions have been compared with observations. The comparison indicates that, for supercritical fast shocks, the three-fluid model can explain cross-shock minor ion heating which is significantly greater than that of protons. When the ratio of specific heats for minor ions, gamma (alpha), equals 2, both the lesser cross-shock deceleration and the greater heating of minor ions than of protons can be predicted by the model; thus, the minor ion heating through the shock transition region is consistent with the involvement of two degrees of freedom. Because the analysis is formulated in the de Heffmann-Teller frame of reference, the method is not valid for perpendicular shocks or when the angle is large. These results agree with the few extant observations and might be confirmed by further observations at the earth's bow shock.

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