Focusing anisotropy of solar cosmic rays

Details Focusing anisotropy of solar cosmic rays Focusing anisotropy of solar cosmic rays

Aug 1986

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986jgr....91.8713b&link_type=abstract

Journal of Geophysical Research (ISSN 0148-0227), vol. 91, Aug. 1, 1986, p. 8713-8724.

Physics

35

Anisotropy, Focusing, Solar Cosmic Rays, Angular Distribution, Boltzmann Transport Equation, Mean Free Path, Transport Theory

Scientific paper

Cosmic ray transport theories that incorporate the effect of adiabatic focusing into the usual pitch angle scattering formalism suggest that the commonly assumed first-order (cosine of pitch angle) anisotropy should be replaced by an exponential function in which the scattering mean free path λ and the index q, which characterizes the dependence of the scattering rate upon pitch angle, appear as parameters. The solar cosmic ray event of February 16, 1984, which exhibited an unusually large, persistent anisotropy, provides an ideal observational basis for testing this theoretical prediction. Analysis of energetic particle data from the International Cometary Explorer and from eight high-latitude neutron monitors indicates that an exponential with λ > 2 AU and with q in the range 1.3 - 1.7 does indeed provide a significantly better description of particle anisotropies than the first-order form. The time profile was shaped primarily by coronal processes. Specifically, coronal diffusion with a rigidity-independent diffusion coefficient ≡1018cm2s-1 and with velocity-dependent escape provides a good fit to both the ICE and the neutron monitor data.

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