B.T. Tsurutani1,3, L.D. Zhang1, Glenn M. Mason2,4, Gurbax Lakhina1, Tohru Hada5, 
John K. Arballo1, Ronald D. Zwickl3

1 Jet Propulsion Laboratory, 4800 Oak Grove Drive, Pasadena, California 91109
2 Department of Physics, University of Maryland, College Park, Maryland 20742
3 National Oceanic and Atmospheric Administration, 
  Space Environment Laboratory, Code R/E/SE, Boulder, Colorado 80303
4 Institute for Physical Science and Technology, 
  University of Maryland, College Park, Maryland 25742
5 ESST Kyushu University, Kasuga 816-8580, Japan

ISEE-3 energetic particles and MHD waves are studied to investigate particle propagation and scattering between the source near the Sun and the Earth (1 AU). For ³He rich events, simultaneous interplanetary magnetic spectra are measured. The interplanetary turbulence through which the particles have traversed is found to be fairly low. This can be interpreted as indicating that either low turbulence fields are necessary for the particles to propagate long (~1.3 AU) distances, or that the fields above active regions producing ³He events have a lack of waves/turbulence. If the former is the case, there may be many ³He events at the sun that are not detected at 1 AU. The largest solar particle events are analyzed to investigate the possibilities of local wave generation at 1 AU. No evidence for wave instability is found at either the leading edge or at the point of peak flux. Our results indicate that interplanetary solar wind "fossil" waves are the important scatterers for particles coming from the Sun to 1 AU, and it is the quiet to intermediate level of IMF activity that are associated with the ³He scatter-free events. Lastly we intercompare the particle mean free paths calculated from resonant wave-particle interactions and from those derived from ³He⁺⁺ intensity and anisotropy time profiles . By including measured wave polarization and wave k directions, we decrease the previously noted discrepancy between and by a factor of ~ 2. We note that is determined by the process of pitch angle scattering from ~ 0° to ~ 180°, while by that from ~ 0° to ~ < 90°. But the scattering across 90° pitch angle is a different process. Therefore the remaining discrepancy between and may lie in the fact that diffusion across 90° pitch angle is much slower than resonant scattering near 0° and 180° pitch angle.