Part II Acceleration Mechanisms of Cosmic Rays
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概要
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The mechanisms of accelerating charged particles in cosmic space are investigated systematically. As the cosmic rays are very commom and important energy-carriers in the universe, the acceleration procedures should be widely operative, including various scales of accelerating regions, various kinds of particles, various intensities of the field, and so on. These characters make it possible to introduce several hierarchy stages in the actual processes. In most cases the charged particles will exchange their energies with the magnetic fields surrounding them in two characteristic ways, secular and statistical. In a secular process a particle gains energy continuously in time and usually it is associated with a rapid process, whereas in a statistical process both the gain and the loss of the energy are possible in a single step of the process but after many steps they are averaged to give a net gain in energy. The statistical processes are most important for understanding the general scope of cosmic ray spectrum, and the acceleration efficiency defined by ε=(damping rate of Alfven wave) (accelerating time) is a chracteristic measurement for each process, while the secular processes are rather peculiar in nature though they will be very effective especially in the injection stage at source regions. The gross feature of the cosmic ray spectrum is naturally introduced from the thermodynamical stand-point in §2. The energy balance among the various modes such as magnetic fields, thermal and turbulent motion of gases, radiations and cosmic rays, is taken into account. As several specific cases, the stationary states, the last phase of source activity and the impulsive energy supply are treated, and the respective spectral indices given by different authors are derived systematically. The dynamical treatment of the acceleration mechanisms is given in §3, where the motion of a charged particle in an externally given electromagnetic field is formulated. The behaviour of a charged particle encountered with moving magnetic irregularities has been discussed by many authors to have concrete models of accelerating processes. The dynamical treatment of this problem leads to the two fundamental processes, the Fermi and the betatron mechanisms, as well as two other rather inefficient ones, the induction and the transit-time accelerations. The Fermi process is a representative of the statistical acceleration, while the betatron process shows, in some cases, secular nature, though in a larger scale the latter should also be combined with the statistical processes. These two are rather closely interrelated and their combination should be taken as the main part of acceleration. In these main processes the motion of individual particles is governed by the adiabatic invariant quantities, i. c. , the gyromagnetic moment, the longitudinal invariant, and the flux invarant. In a rapidly changing magnetic field, however, they are no Ionger. conserved and as a result some secular accelerations become possible. The induction acceleration is given as a non-adiabatic betatron effect and will be effective in certain cases as is illustrated. ln order to analyse various actual accelerating regions, the combined Fermi and betatron processes are assumed in §4. The relative rates of these two processes give rise to a chararacteristic rigidity spectrum and an A / Z dependence. If the chemical composition of the cosmic ray source is maintained by the relative intensities of nuclear particles of cosmic rays, while the electron intensity is much less than the proton intensities observed in cosmic rays, then one would have a condition for the relative rates of the Fermi and the betatron accelerations, a and b, mc^2<(b / a)^22kT<Mc^2, where T is the source temperature for both electrons and protons, and m and M respectively denote the masses of the electron and the proton. The rigidity spectra of the solar cosmic rays clearly show the above characters. (§4・3 a
- 理論物理学刊行会の論文
著者
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Sato Humitaka
Department Of Physics Kyoto Univesity
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Sato Humitaka
Department Of Nuclear Science Kyoto University
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NISHIMURA Jun
Institue of Space and Astronautical Science, Japan Aerospace Exploration Agency
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Nishimura Jun
Institue Of Space And Astronautical Sci. Japan Aerospace Exploration Agency
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Hayakawa Satio
Department Of Physics Nagoya University
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OBAYASHI Haruo
Department of Physics, Nagoya University
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Hayakawa Satio
Department Of Astrophysics Faculty Of Science Nagoya University
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Obayashi Haruo
Department Of Physics Nagoya University
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Nishimura Jun
Institute For Nuclear Study University Of Tokyo
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SATO Humitaka
Department of Nuclear Science, Kyoto University
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