Study of energetic solar particle events of 18 November 1968, 25 February 1969, and 30 March 1969

The solar particle events of 18 November 1968, 25 February 1969, and 30 March 1969 were studied using data from the detector system aboard the lunar orbiting satellite Explorer 35. Protons, alpha particles, and Z or = 3 nuclei were registered in the solid state detector of the system. Interplanetary propagation, particle anisotropy, and the intensity ratios of protons to alpha particles and of alpha particles to C, N, and O nuclei above a common specific energy of 0.5 MeV/nucleon were studied. Diffusion coefficients and decay constants for the three events are given, as well as magnitudes and directions of anisotropies

The geomagnetic cavity and the Van Allen radiation belts (Van Allen radiation belt particle motion in spherically confined magnetosphere)

The StxF6;rmer's study is extended to examine the motion of a charged particle in a spherically confined magnetosphere. It is shown that the x2018;allowedx2019; region computed on this basis for proton energies ranging from 10 to 710 MeV is in a close agreement with the radial distribution and latitude dependence of the inner zone. A similar study is made also for electrons in the energy range 10x2013;900 keV

The geomagnetic cavity and the Van Allen radiation belts

The StŌrmer's study is extended to examine the motion of a charged particle in a spherically confined magnetosphere. It is shown that the 'allowed' region computed on this basis for proton energies ranging from 10 to 710 MeV is in a close agreement with the radial distribution and latitude dependence of the inner zone. A similar study is made also for electrons in the energy range 10-900 keV

The Geomagnetic cavity and the Van Allen radiation belts-II

Using the spherical harmonic expansion given by Mead for the magnetic field created by the currents on the surface of the geomagnetic cavity, the nature of the trapping regions has been discussed. It is shown that to a first order of approximation in the expansion coefficients, the allowed regions are still determined by a cubic equation. Numerical determinations have been made for the structure of the allowed regions for particles of different energies both on the sunlit side as well as the dark side of the Earth.13