The time‐dependent flux of equatorial electrons (0.4 Mev ≲ E ≲ 2.2 Mev) observed on ATS 1 often exhibits drift‐periodic structures that can be traced back to a sudden expansion or compression of the magnetosphere. The magnetospheric disturbance redistributes the energetic electrons among drift shells in an asymmetrical manner, and this spatial asymmetry between noon and midnight reveals itself as a temporal variation in particle flux as the electrons subsequently drift past the observer. A mathematical model for the dynamics of this azimuthal bunching of energetic electrons reveals the microstructure of the redistribution of electrons among drift shells and indicates qualitatively the relation of this microstructure to the diffusion of particles across L.
Theoretical expressions for both the nonrelativistic and relativistic nuclear matrix elements for /3 transitions of arbitrary forbiddenness are derived by using the Nilsson model. The /3-decay operators are expressed in terms of irreducible spherical tensors. One-and two-particle intrinsic wave functions are used for odd-and even-mass nuclei, respectively. For even-mass nuclei, the results are found to be strongly dependent on the coupling of the two particles. The results are expected to be applicable to decays involving both intrinsic ground states and excited intrinsic states. The theoretical expressions are used to calculate matrixelement parameters for/? decays in Tm 170 and Re 186 . The theoretical values are compared with experimentally determined values of the Tm 170 and Re 186 parameters.
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