| 书目名称 | Cosmic Ray Astrophysics | | 编辑 | Reinhard Schlickeiser | | 视频video | | | 概述 | This is the only modern book on the market.All competitive titles date back to 1990 and do not take the latest developments into account.Includes supplementary material: | | 丛书名称 | Astronomy and Astrophysics Library | | 图书封面 |  | | 描述 | This book provides an exhaustive account of the origin and dynamics of cosmic rays. Divided into three parts, it first gives an up-to-date summary of the observational data, then -- in the following theory section -- deals with the kinetic description of cosmic ray plasma. The underlying diffusion-convection transport equation, which governs the coupling between cosmic rays and the background plasma, is derived and analyzed in detail. In the third part, several applications of the solutions of the transport equation are presented and how key observations in cosmic ray physics can be accounted for is demonstrated. The applications include cosmic ray modulation, acceleration near shock waves and the galactic propagation of cosmic rays. While the book is primarily of interest to scientists working at the forefront of research, the very careful derivations and explanations make it suitable also as an introduction to the field of cosmic rays for graduate students. | | 出版日期 | Textbook 2002 | | 关键词 | astrophysics; cosmic ray; cosmic rays; electron; particle astrophysics; planet; plasma waves; radiation; uni | | 版次 | 1 | | doi | https://doi.org/10.1007/978-3-662-04814-6 | | isbn_softcover | 978-3-642-08573-4 | | isbn_ebook | 978-3-662-04814-6Series ISSN 0941-7834 Series E-ISSN 2196-9698 | | issn_series | 0941-7834 | | copyright | Springer-Verlag Berlin Heidelberg 2002 |
| 1 |
Front Matter |
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Abstract
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| 2 |
,Introduction, |
Reinhard Schlickeiser |
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Abstract
At six o’clock on the morning of August 7, 1912, the Austrian physicist Victor Hess and two companions climbed into a balloon gondola for the last of a series of seven launches. The flight, which had started at Aussig on the river Elbe, was under the command of Captain W. Hoffory. The meteorological observer was W. Wolf and Hess listed himself as “observer for atmospheric electricity”. Over the next three or four hours the balloon rose to an altitude above 5 km, and by noon the group was landing at Pieskow, some 50 km from Berlin. During the six hours of flight Hess had carefully recorded the readings of three electroscopes he used to measure the intensity of radiation and had noted a rise in the radiation level as the balloon rose in altitude.
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| 3 |
,Cosmic Rays as Part of the Universe, |
Reinhard Schlickeiser |
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Abstract
In the preceding introductory chapter cosmic radiation has been defined as extraterrestrial charged particle radiation, i.e. it consists of a flux of electrons, positrons and nucleons with kinetic energies greater than 1 keV that bombards the Earth from outside. To understand the origin and dynamics of these particles we have to recall some basic astronomical observations concerning the structure and content of the universe.
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| 4 |
,Direct Observations of Cosmic Rays, |
Reinhard Schlickeiser |
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Abstract
With the technical capability of flying balloons high in the Earth atmosphere and launching satellites into extraterrestrial space carrying light-weight solid-state particle detectors, which was achieved after World War II, the original ground-based cosmic ray airshower experiments were supplemented by in situ measurements of the cosmic ray flux in the interplanetary space. Today, detectors on board spacecraft routinely provide spatial and temporal information on the particle energy spectra throughout the heliosphere.
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| 5 |
,Interactions of Cosmic Ray Electrons, |
Reinhard Schlickeiser |
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Abstract
Because of the influence of non-uniform cosmic magnetic fields it is impossible to observe directly the intensity of cosmic rays in regions of the Universe other than the neighborhood of our solar system. However, by measuring the electromagnetic radiation that results from interactions of cosmic rays with other constituents of the Universe we can infer the cosmic ray intensity in other regions of space. Since neutrino astronomy is still in its infancy this is the only method existing today. This chapter is devoted to a discussion of the radiation and interaction processes of cosmic ray electrons. In the next chapter we will discuss the radiation and interaction processes of cosmic ray nucleons. The purposes of these two chapters are two-fold. First, we want to investigate the influence of these interaction processes on the dynamics of the cosmic rays. As the particles interact and produce observable electromagnetic radiation they continuously lose energy and that should affect their propagation and their original energy spectrum. Second, we want to establish the relation between the observable electromagnetic radiation spectra and properties of the radiating particles. Armed with
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| 6 |
,Interactions of Cosmic Ray Nuclei, |
Reinhard Schlickeiser |
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Abstract
In Chap. 4 we have seen that the cross-sections for point-like electromagnetic interactions of cosmic ray electrons (synchrotron radiation, inverse Compton scattering, nonthermal bremsstrahlung) involve the Thomson cross-section being proportional to the square of the electron radius of the radiating particle. Therefore, if we consider here a heavy cosmic ray nucleus of charge . and mass .. instead of a cosmic ray electron, the corresponding cross-sections involve the square of the nucleon radius .. - (.)./(....) = (../.)(../..).. yielding the Thomson cross-section for nuclei. As a consequence the cross-sections of electromagnetic interactions of cosmic ray nucleus are much smaller than those of the cosmic ray electrons of the same Lorentz factor, and can be neglected in practically all astrophysical applications as production processes for cosmic photons and as energy loss processes for cosmic ray nuclei.
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| 7 |
,Indirect Observations of Cosmic Rays, |
Reinhard Schlickeiser |
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Abstract
The measured frequency spectrum of electromagnetic radiation from a cosmic object provides clues on the presence and the properties of the radiating cosmic ray particles once the radiation process and the source geometry are specified. As discussed in Chaps. 4 and 5 for cosmic ray electrons synchrotron radiation in the radio wavelength band and for cosmic ray nuclei emission at γ-ray frequencies are most decisive. In the following we describe the results from radio and γ-ray astronomy concerning the origin of cosmic rays.
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| 8 |
,Immediate Consequences of Galactic Cosmic Ray Observations, |
Reinhard Schlickeiser |
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Abstract
Summarizing the observational material on galactic cosmic rays presented in the last three chapters we note that the solar system is bombarded by cosmic rays from all sides isotropically. The chemical and isotopic composition of the nucleonic component is similar to that of solar flare particles; all nucleons exhibit power law energy spectra over a wide range of kinetic energies. Cosmic ray electrons exhibit a break in their power law energy spectrum at about 20 GeV with spectral index ≃ 2.2 below the break energy and ≃ 3.2 above the break energy.
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| 9 |
,Statistical Mechanics of Charged Particles, |
Reinhard Schlickeiser |
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Abstract
As we have seen in Chap. 2 most of the non-stellar matter in the universe is ionized, and therefore the statistical mechanics of charged particles and their mutual interactions via electromagnetic fields, generated and maintained by their own streaming, is of particular importance not only for the cosmic rays but also the other components of the interstellar and intergalactic media. In this chapter we will consider the behavior of an electrically neutral (on the average) system of charged and neutral particles interacting with each other and with an external magnetic field. A gas containing so many free charged particles that their collective Lorentz forces influence the properties of the medium considerably is referred to as a ..
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| 10 |
,Test Wave Approach 1. Waves in Cold Magnetized Plasmas, |
Reinhard Schlickeiser |
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Abstract
According to the kinetic theory of plasma waves (Sect. 8.3) the electromagnetic fluctuations in a given initial configuration (..., .., ..), after an initial transit period, will consist of a spectrum of normal modes at different wavenumbers, see (8.3.42). In the following we will discuss the resulting plasma waves for different assumed initial configurations of magnetized plasma. After treating plasma waves in cold and hot plasmas in this and the next chapter we are ready to investigate the situation characteristics for cosmic rays in space plasmas, where relativistic cosmic rays co-exist with a background interstellar or intergalactic plasma.
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| 11 |
,Test Wave Approach 2. Waves in Hot Magnetized Isotropic Plasmas, |
Reinhard Schlickeiser |
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Abstract
According to the kinetic theory of plasma waves (Sect. 8.3) the electromagnetic fluctuations in a given initial configuration (..., .., ..), after an initial transit period, will consist of a spectrum of normal modes at different wavenumbers, see (8.3.42). After discussing the cold plasma limit in the last chapter we now turn our attention to hot plasmas.
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| 12 |
,Test Wave Approach 3. Generation of Plasma Waves, |
Reinhard Schlickeiser |
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Abstract
In this chapter we will study particle distribution functions ..(.) that lead to solutions of the dispersion relation with . values of the imaginary part of the wave frequency, . > 0, and thus give rise to growing fluctuations. We will start out from the classical two-stream instability and then study in detail cosmic-ray-induced instabilities.
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| 13 |
,Test Particle Approach 1. Hierarchy of Transport Equations, |
Reinhard Schlickeiser |
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Abstract
After having established the nature and sources of cosmic plasma waves we now turn to the effect of these plasma waves on the cosmic rays.
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| 14 |
,Test Particle Approach 2. Calculation of Transport Parameters, |
Reinhard Schlickeiser |
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Abstract
In the preceding chapter we have developed the quasilinear theory for calculating the cosmic ray transport parameters for arbitrary plasma wave turbulence. As we have learned from the streaming instability studies in Sect. 11.2 in particular low-frequency Alfvén waves and magnetosonic waves, described by the dispersion relations (9.2.63), have short growth times in cosmic plasmas. We therefore calculate the cosmic ray transport parameters (12.3.24)–(12.3.30) for these two plasma modes. The plasma wave properties enter the Fokker-Planck coefficients through the electric and magnetic field correlation functions (12.2.6) which for individual plasma modes are related because of Maxwell’s induction law (12.2.9).
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| 15 |
,Acceleration and Transport Processes of Cosmic Rays, |
Reinhard Schlickeiser |
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Abstract
Essential to an explanation of most phenomena of high-energy astrophysics is the understanding of the physics of the acceleration and transport of the energetic charged particles, i.e. the cosmic rays. The in-situ study of these transport and acceleration processes in interplanetary space offers a unique opportunity to test our conceptual understanding of cosmic ray dynamics, and thus provides an increased confidence in the applicability of the developed concepts. The transport and acceleration of cosmic rays in interplanetary space are quite similar to those in other cosmic objects. Quite generally, the cosmic ray particles have to propagate in a collisionless, high-conductive, magnetized and tenuous background plasma consisting mainly of protons and electrons. Very often the energy density of cosmic ray particles is comparable to that of the background medium, the magnetic field and the convective motion of the medium. As a consequence, the electromagnetic fields in the system are severely influenced by the cosmic ray particles, and the description of cosmic ray transport and acceleration is more complex than solving the equation of motion of charged cosmic ray test particles in
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| 16 |
,Interplanetary Transport of Cosmic Ray Particles, |
Reinhard Schlickeiser |
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Abstract
We have demonstrated in Chaps. 12 and 13 that the quasilinear cosmic ray transport parameters in a given astrophysical system are determined by the statistical properties of the electromagnetic fluctuations in this system, expressed through the correlation tensors of the electric and magnetic field fluctuations (12.2.6). If these electromagnetic fluctuations can be identified with normal low-frequency plasma wave modes and/or exhibit certain symmetry properties with respect to the uniform background magnetic field, the calculation of the cosmic ray transport parameters simplifies enormously under the diffusion approximation, as shown in Chap. 13.
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发表于 2025-3-21 20:09:41
