Stream interfaces and energetic ions closer than expected: Analyses of Pioneers 10 and 11 observations

Details Stream interfaces and energetic ions closer than expected: Analyses of Pioneers 10 and 11 observations Stream interfaces and energetic ions closer than expected: Analyses of Pioneers 10 and 11 observations

Jun 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994georl..21.1117i&link_type=abstract

Geophysical Research Letters (ISSN 0094-8276), vol. 21, no. 12, p. 1117-1120

Physics

19

Corotation, Energetic Particles, Interfaces, Ions, Reversed Flow, Shock Waves, Solar Rotation, Solar Wind, Spatial Distribution, Magnetohydrodynamics, Mathematical Models, Pioneer 10 Space Probe, Pioneer 11 Space Probe, Prediction Analysis Techniques, Solar Probes

Scientific paper

An empirical study of corotating interaction regions (CIRs) observed between 3.9 AU and 5.9 AU on Pioneers 10 and 11 shows that the main corotation energetic ion population (CEIP), which is associated with the trailing reverse shock, terminates within the CIR at a definite, structural boundary, which we show here is the stream interface. This new result has significant implications for solar wind and energetic particle modeling. In particular it implies either that the reverse shock forms closer to the stream interface than models suggest or that the theories that treat the generation and transport of these energetic ions, such as preshock Fermi acceleration and cross-field diffusion must be combined or extended. We test these scenarios by comparing the CEIP intensity profiles on the two sides of the stream interface. We find that while each automatically accounts for one or two aspects of the results none of them alone can account for all of our empirical results.

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