Correlation between energetic ion enhancements and heliospheric current sheet crossings in the outer heliosphere

J. D. Richardson, E. C. Stone, A. C. Cummings, J. C. Kasper, M. Zhang, L. F. Burlaga, N. F. Ness, Y. Liu

doi:10.1029/2006gl027578

Correlation between energetic ion enhancements and heliospheric current sheet crossings in the outer heliosphere

DOI Web Site Web Site 被引用文献1件

J. D. Richardson

Center for Space Research Massachusetts Institute of Technology Cambridge Massachusetts USA
E. C. Stone

Division of Physics, Mathematics, and Astronomy California Institute of Technology Pasadena California USA
A. C. Cummings

Division of Physics, Mathematics, and Astronomy California Institute of Technology Pasadena California USA
J. C. Kasper

Center for Space Research Massachusetts Institute of Technology Cambridge Massachusetts USA
M. Zhang

Department of Physics and Space Sciences Florida Institute of Technology Melbourne Florida USA
L. F. Burlaga

Laboratory for Solar and Space Physics NASA Goddard Space Flight Center Greenbelt Maryland USA
N. F. Ness

Bartol Research Institute University of Delaware Newark Delaware USA
Y. Liu

Center for Space Research Massachusetts Institute of Technology Cambridge Massachusetts USA

書誌事項

公開日: 2006-11

権利情報

http://onlinelibrary.wiley.com/termsAndConditions#vor

DOI

10.1029/2006gl027578

公開者: American Geophysical Union (AGU)

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説明

<jats:p>Voyagers 1 and 2 observed highly‐variable beams of energetic ions in the foreshock region upstream of the termination shock (TS). At Voyager 2 (V2), the ion intensities are generally not related to the plasma properties. At Voyager 1 (V1), the beams are often coincident with crossings of the heliospheric current sheet (HCS). The V1 intensity peaks occur when the HCS is crossed from negative to positive magnetic polarities and V1 is within a few AU of the TS. Two mechanisms are considered: current sheet drift and streaming of ions from the TS along magnetic field lines which are parallel to the HCS. The current sheet drift hypothesis predicts that enhancements observed at V2 will occur when the HCS is crossed in the opposite direction, from positive to negative magnetic polarity, since V2 is at southern heliolatitudes.</jats:p>