The heliospheric modulation of 3-10 MeV electrons: Modeling of changes in the solar wind speed in relation to perpendicular polar diffusion

[1]  A. Shalchi,et al.  Nonlinear Parallel and Perpendicular Diffusion of Charged Cosmic Rays in Weak Turbulence , 2004 .

[2]  B. Heber,et al.  Out‐of‐ecliptic quiet time MeV electron increases: Ulysses COSPIN/KET observations , 2004 .

[3]  R. Schlickeiser,et al.  The Parallel Mean Free Path of Heliospheric Cosmic Rays in Composite Slab/Two-dimensional Geometry. I. The Damping Model of Dynamical Turbulence , 2004 .

[4]  B. Heber,et al.  Solar Wind Effects on the Transport of 3-10 MeV Cosmic-Ray Electrons from Solar Minimum to Solar Maximum , 2003 .

[5]  B. Heber,et al.  Transport of a few-MEV jovian and galactic electrons at solar maximum , 2003 .

[6]  B. Heber,et al.  Quiet time MEV electron increases at solar maximum: Ulysses cospin/ket observations , 2003 .

[7]  B. Heber,et al.  Particle drift effects on cosmic ray modulation during solar maximum , 2003 .

[8]  M. Potgieter,et al.  Modulation effects of a changing solar wind speed on low-energy electrons , 2003 .

[9]  W. Matthaeus,et al.  Nonlinear Collisionless Perpendicular Diffusion of Charged Particles , 2003 .

[10]  B. Heber,et al.  3-20 MeV Electrons in the Inner Three-dimensional Heliosphere at Solar Maximum: Ulysses COSPIN/KET Observations , 2002 .

[11]  R. Skoug,et al.  Ulysses' second fast‐latitude scan: Complexity near solar maximum and the reformation of polar coronal holes , 2002 .

[12]  B. Heber,et al.  Modulation of Jovian and galactic electrons in the heliosphere: 2. Radial transport of a few MeV electrons , 2001 .

[13]  B. Heber,et al.  Rigidity dependence of cosmic ray proton latitudinal gradients measured by the Ulysses spacecraft: Implications for the diffusion tensor , 2000 .

[14]  H. Fichtner,et al.  On the propagation of Jovian electrons in the heliosphere: Transport modelling in 4‐D phase space , 2000 .

[15]  S. Bravo,et al.  The 22-yr modulation of galactic cosmic rays and its relation to coronal holes , 1996 .

[16]  S. Suess,et al.  Ulysses solar wind plasma observations from pole to pole , 1995 .

[17]  N. Gehrels,et al.  Voyager 2: Energetic Ions and Electrons in the Jovian Magnetosphere , 1979, Science.

[18]  N. Gehrels,et al.  Voyager 1: Energetic Ions and Electrons in the Jovian Magnetosphere , 1979, Science.

[19]  E. Roelof,et al.  Interplanetary Mev electrons of Jovian origin , 1974 .

[20]  J. Simpson,et al.  Protons and Electrons in Jupiter's Magnetic Field: Results from the University of Chicago Experiment on Pioneer 10 , 1974, Science.

[21]  E. Roelof,et al.  A coronal hole and its identification as the source of a high velocity solar wind stream , 1973 .

[22]  W. Dröge.  Probing heliospheric diffusion coefficients with solar energetic particles , 2004 .

[23]  D. Moeketsi.  Modelling of galactic and jovian electrons in the heliosphere , 2004 .

[24]  J. Richardson,et al.  The solar wind: from solar minimum to solar maximum , 2001 .

[25]  J. Jokipii,et al.  Modeling of 3-D Corotating Cosmic-Ray Structures in the Heliosphere , 1998 .

[26]  F. Tsuchiya,et al.  Modulation of Jovian electrons by the solar wind , 1997 .

[27]  Eugene N. Parker,et al.  THE PASSAGE OF ENERGETIC CHARGED PARTICLES THROUGH INTERPLANETARY SPACE , 1965 .