Proton and electron mean free paths: The Palmer consensus revisited

Charge sign dependence of cosmic ray modulation near a rigidity of 1 GV

“…There is also a major velocity difference between electrons and helium. Recently, interest in velocity as a parameter in its own right has increased with the development of dynamic models of particle scattering in the interplanetary magnetic field [Bieber et al, 1994]. …”

Transport of solar wind fluctuations: A two-component model

“…[2] Fluctuations in the velocity and magnetic fields of the solar wind play important roles in various processes in the heliosphere, including scattering of solar energetic particles [Bieber et al, 1994;Dröge et al, 2010], modulation of galactic cosmic rays [Zank et al, 1998;Pei et al, 2010], and heating of the solar wind itself [Coleman, 1968;Matthaeus et al, 1999;Cranmer and van Ballegooijen, 2003]. The spatial transport and evolution of these fluctuations is thus a topic of some importance in heliospheric physics.…”

The Ace Magnetic Fields Experiment

“…However, there is growing evidence that 80 of the magnetic uctuation energy is carried by t wo-dimensional 2-D turbulence that is self-organized and oriented at right angles relative to the large-scale magnetic eld Matthaeus et al, 1990;Zank and Matthaeus, 1992;Bieber et al, 1996 and there is some evidence that interaction between 2-D turbulence and thermal particles is signi cant Ambrosiano et al, 1988 . Preliminary analyses show that such 2-D uctuations show v ery little interaction with energetic particles in the quasilinear limit Bieber et al, 1994 , but quite compelling evidence exists that even a small percentage of 2-D turbulence can lead to a signi cant degree of eld line di usion Matthaeus et al, 1995;Gray et al, 1996 which, in turn, leads to energetic charged particle di usion. Consideration of such 2-D uctuations have brought quasilinear theory into agreement with observed cosmic ray mean-freepaths while magnetodynamic revisions of the familiar magnetostatic quasilinear theory coupled to consideration of the smallest scale uctuations that form the dissipation range of IMF turbulence has proven successful in accounting for the observed charge-dependent scattering rates of protons and electrons Bieber et al, 1994 .…”

“…Preliminary analyses show that such 2-D uctuations show v ery little interaction with energetic particles in the quasilinear limit Bieber et al, 1994 , but quite compelling evidence exists that even a small percentage of 2-D turbulence can lead to a signi cant degree of eld line di usion Matthaeus et al, 1995;Gray et al, 1996 which, in turn, leads to energetic charged particle di usion. Consideration of such 2-D uctuations have brought quasilinear theory into agreement with observed cosmic ray mean-freepaths while magnetodynamic revisions of the familiar magnetostatic quasilinear theory coupled to consideration of the smallest scale uctuations that form the dissipation range of IMF turbulence has proven successful in accounting for the observed charge-dependent scattering rates of protons and electrons Bieber et al, 1994 .…”