THE INFLUENCE OF KLEIN-NISHINA STEPS ON THE SPATIAL DIFFUSION OF GALACTIC COSMIC-RAY ELECTRONS

被引:7
作者
Blies, P. [1 ]
Schlickeiser, R. [1 ]
机构
[1] Ruhr Univ Bochum, Lehrstuhl Weltraum & Astrophys 4, Inst Theoret Phys, D-44780 Bochum, Germany
关键词
cosmic rays; diffusion; radiation mechanisms: non-thermal; SYNCHROTRON-RADIATION; TRANSPORT; PROPAGATION; ENERGIES; EQUATION; CROSS;
D O I
10.1088/0004-637X/751/1/71
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
The fullKlein-Nishina cross section for the inverse Compton scattering interactions of electrons implies a significant reduction of the electron energy loss rate compared to the Thomson limit when the electron energy exceeds the critical Klein-Nishina energy E-K = 0.27m(e)(2)c(4)/(k(B)T),where T denotes the temperature of the photon graybody distribution. We investigate the influence of the Klein-Nishina reduction on the solution of the steady-state spatial diffusion transport equation for relativistic electrons. The modified electron spectrum at energies below 10(4) GeV, where only the Klein-Nishina modifications from interstellar optical target photons are relevant, are derived in terms of the Green's function solution for one-, two-, and three-dimensional spatial diffusion. The modifications to the solutions of the one- and three-dimensional diffusion equations are calculated for a single point source of monoenergetic electrons. It is shown that significant enhancements in the local electron intensity occur at electron energies greater than the critical Klein-Nishina energy E-K, and that the cosmic-ray electron anisotropy at the solar system resulting from a single steady point source exhibits a sharp drop near E-K. These Klein-Nishina enhancements are potentially interesting for determining the contribution of point sources such as dark matter sources and/or electromagnetic particle accelerators (pulsars and micro-quasars) to the local electron intensity and the local positron fraction.
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页数:7
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