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pursued, because it is in this energy window, through which the acceleration
of UPI to become ACR is best studied, especially, in direct comparison with
ACR measurements at 1 AU, to yield a self-consistent study of charged-
particle acceleration and cosmic-ray modulation in the heliosphere.
31
The
technology is available, only the opportunity is lacking.
37
Acknowledgments
Hearty thanks go to A. Czechowski, M. Gruntman, V. Izmodenov,
R. Kallenbach, and E. Roelof for helpful discussions and for illuminating
figures used for the invited talk, on which this paper is based.
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