The Gradient/Curvature Drift of Cosmic Rays in the Heliospheric Magnetic Fields with Turbulence

Details The Gradient/Curvature Drift of Cosmic Rays in the Heliospheric Magnetic Fields with Turbulence The Gradient/Curvature Drift of Cosmic Rays in the Heliospheric Magnetic Fields with Turbulence

Dec 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004agufmsh43a1099b&link_type=abstract

American Geophysical Union, Fall Meeting 2004, abstract #SH43A-1099

Physics

7859 Transport Processes, 7863 Turbulence, 2104 Cosmic Rays, 2114 Energetic Particles, Heliospheric (7514), 2194 Instruments And Techniques

Scientific paper

Although various observations of cosmic ray modulation indicate that the effects of gradient/curvature particle drift should be reduced from its full drift in the average Parker heliospheric magnetic field, there is no theory for the calculation of particle drift in a magnetic field with turbulence. We present here a new approach to this problem, using an orbit tracing method for the calculation of drift. The solution is a direct numerical integration of the basic expression for drift as presented in Rossi and Olbert [1970]. The same technique was previously used to calculate the drifts in the Parker field for particles with an isotropic distribution. The drift speed agrees with the first order drift approximation when the particle gyroradius is much less than the scale size of magnetic field gradient. In this case, we include a more complicated magnetic field which contains both slab and 2D components of turbulence [Bieber et al, 1994; Qin et al, 2002]. It is expected that the turbulence will alter the particle trajectory, thus changing the behavior of the particle drift. Its implications to cosmic ray modulation will also be discussed

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