等离子体天体物理学,第一部分

出版时间：2012-12  出版社：北京大学出版社  作者：索莫夫  页数：437  

内容概要

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作者简介

作者：（俄罗斯）索莫夫（Somov B.V.）

书籍目录

About This Book Plasma Astrophysics: History and Neighbours Particles and Fields: Exact Self-Consistent Description 1.1 Interacting particles and Liouville's theorem 1.1.1 Continuity in phase space 1.1.2 The character of particle interactions 1.1.3 The Lorentz force, gravity 1.1.4 Collisional friction in plasma 1.1.5 The exact distribution function 1.2 Charged particles in the electromagnetic field 1.2.1 General formulation of the problem 1.2.2 The continuity equation for electric charge 1.2.3 Initial equations and initial conditions 1.2.4 Astrophysical plasma applications  1.3 Gravitational systems 1.4 Practice: Exercises and Answers 2 Statistical Description of Interacting Particle Systems 2.1 The averaging of Liouville's equation 2.1.1 Averaging over phase space 2.1.2 Two statistical postulates 2.1.3 A statistical mechanism of mixing in phase space  2.1.4 The derivation of a general kinetic equation 2.2 A collisional integral and correlation functions 2.2.1 Binary interactions 2.2.2 Binary correlation 2.2.3 The collisional integral and binary correlation 2.3 Equations for correlation functions 2.4 Practice: Exercises and Answers Weakly-Coupled Systems with Binary Collisions 3.1 Approximations for binary collisions 3.1.1 The small parameter of kinetic theory 3.1.2 The Vlasov kinetic equation 3.1.3 The Landau collisional integral 3.1.4 The Fokker-Planck equation 3.2 Correlation function and Debye shielding 3.2.1 The Maxwellian distribution function 3.2.2 The averaged force and electric neutrality 3.2.3 Pair correlations and the Debye radius 3.3 Gravitational systems 3.4 Comments on numerical simulations 3.5 Practice: Exercises and Answers Propagation of Fast Particles in Plasma 4.1 Derivation of the basic kinetic equation 4.1.1 Basic approximations 4.1.2 Dimensionless kinetic equation in energy space 4.2 A kinetic equation at high speeds 4.3 The classical thick-target model 4.4 The role of angular diffusion 4.4.1 An approximate account of scattering 4.4.2 The thick-target model 4.5 The reverse-current electric-field effect 4.5.1 The necessity for a beam-neutralizing current 4.5.2 Formulation of a realistic kinetic problem 4.5.3 Dimensionless parameters of the problem 4.5.4 Coulomb losses of energy 4.5.5 New physical results 4.5.6 To the future models 4.6 Practice: Exercises and Answers Motion of a Charged Particle in Given Fields 5.1 A particle in constant homogeneous fields 5.1.1 Relativistic equation of motion 5.1.2 Constant non-magnetic forces 5.1.3 Constant homogeneous magnetic fields 5.1.4 Non-magnetic force in a magnetic field 5.1.5 Electric and gravitational drifts 5.2 Weakly inhomogeneous slowly changing fields 5.2.1 Small parameters in the motion equation 5.2.2 Expansion in powers of m/e 5.2.3 The averaging over gyromotion 5.2.4 Spiral motion of the guiding center 5.2.5 Gradient and inertial drifts 5.3 Practice: Exercises and Answers Adiabatic Invariants in Astrophysical Plasma 6.1 General definitions 6.2 Two main invariants 6.2.1 Motion in the Larmor plane 6.2.2 Magnetic mirrors and traps 6.2.3 Bounce motion 6.2.4 The Fermi acceleration 6.3 The flux invariant 6.4 Approximation accuracy. Exact solutions 6.5 Practice: Exercises and Answers Wave-Particle Interaction in Astrophysical Plasma 7.1 The basis of kinetic theory 7.1.1 The linearized Vlasov equation 7.1.2 The Landau resonance and Landau damping 7.1.3 Gyroresonance 7.2 Stochastic acceleration of particles by waves 7.2.1 The principles of particle acceleration by waves  7.2.2 The Kolmogorov theory of turbulence 7.2.3 MHD turbulent cascading 7.3 The relativistic electron-positron plasma 7.4 Practice: Exercises and Answers Coulomb Collisions in Astrophysical Plasma 8.1 Close and distant collisions 8.1.1 The collision parameters 8.1.2 The Rutherford formula 8.1.3 The test particle concept 8.1.4 Particles in a magnetic trap 8.1.5 The role of distant collisions 8.2 Debye shielding and plasma oscillations 8.2.1 Simple illustrations of the shielding effect 8.2.2 Charge neutrality and oscillations in plasma 8.3 Collisional relaxations in cosmic plasma 8.3.1 Some exact solutions 8.3.2 Two-temperature plasma in solar flares 8.3.3 An adiabatic model for two-temperature plasma  8.3.4 Two-temperature accretion flows 8.4 Dynamic friction in astrophysical plasma 8.4.1 The collisional drag force and energy losses 8.4.2 Electric runaway 8.4.3 Thermal runaway in astrophysical plasma 8.5 Practice: Exercises and Answers 9 Macroscopic Description of Astrophysical Plasma 9.1 Summary of microscopic description 9.2 Transition to macroscopic description 9.3 Macroscopic transfer equations 9.3.1 Equation for the zeroth moment 9.3.2 The momentum conservation law 9.3.3 The energy conservation law 9.4 General properties of transfer equations 9.4.1 Divergent and hydrodynamic forms 9.4.2 Status of conservation laws 9.5 Equation of state and transfer coefficients 9.6 Gravitational systems 9.7 Practice: Exercises and Answers 10 Multi-Fluid Models of Astrophysical Plasma 10.1 Multi-fluid models in astrophysics 10.2 Langmuir waves 10.2.1 Langmuir waves in a cold plasma 10.2.2 Langmuir waves in a warm plasma 10.2.3 Ion effects in Langmuir waves  10.3 Electromagnetic waves in plasma 10.4 What do we miss? 10.5 Practice: Exercises and Answers 11 The Generalized Ohm's Law in Plasma 11.1 The classic Ohm's law 11.2 Derivation of basic equations 11.3 The general solution 11.4 The conductivity of magnetized plasma 11.4.1 Two limiting cases 11.4.2 The physical interpretation 11.5 Currents and charges in plasma 11.5.1 Collisional and collisionless plasmas 11.5.2 Volume charge and quasi-neutrality 11.6 Practice: Exercises and Answers 12 Single-Fluid Models for Astrophysical Plasma 12.1 Derivation of the single-fluid equations 12.1.1 The continuity equation 12.1.2 The momentum conservation law in plasma 12.1.3 The energy conservation law 12.2 Basic assumptions and the MHD equations 12.2.1 Old and new simplifying assumptions 12.2.2 Non-relativistic magnetohydrodynamics 12.2.3 Relativistic magnetohydrodynamics …… 13 Magnetohydrodynamics in Astrophysics 14 Plasma Flows in a Strong Magnetic Field 15 MHD Waves in Astrophysical Plasma 16 Discontinuous Flows in a MHD Medium 17 Evolutionarity of MHD Discontinuities 18 Particle Acceleration by Shock Waves 19 Plasma Equilibrium in Magnetic Field 20 Stationary Flows in a Magnetic Field Appendix 1. Notation Appendix 2. Useful Expressions Appendix 3. Constants Bibliography Index

章节摘录

版权页：   插图：   These conditions seem to be approximatelly satiesfied in cluster environments;for more detail see Fox and Loeb (1997). The general case of a strong shock in a fully ionized plasma with heatconduction is complicated by the fact that the electron thermal speed exceedsthe shock speed, allowing the electrons to preheat the plasma ahead of theshock (Zel'dovich and Raizer, 1966). Usually heat conduction determinesinternal scales of the problem being in competition with the thermalinstability driven by radiative cooling (Field, 1965; see also Somov and Sy-rovatskii, 1976a). Radiation emitted by the high-temperature plasma behindthe shock also may heat a preshock region. Fast particles, escaping from thehigh-tempertature plasma (see Section 8.4.3), may contribute the preshockheating too. So we have to be very careful when we apply the adiabaticmodel of two-temperature plasma to astrophysical conditions. If come back to HXR tails observed in the X-ray spectra of some clus-ters, one suggestion is that all or part of this emission might be nonthermalbremsstrahlung from suprathermal electrons with energies of ~ 10- 100 keV.This nonthermal electrons would form a population in excess of the normalthermal gas, which is the bulk of the intracluster medium. The most naturalexplanation of this suprathermal population would be that they are particlescurrently being accelerated to high energies by turbulence in the intraclns-ter medium. Sarazin and Kempner (2000) have calculated models for thenonthermal HXR bremsstrahlung in the clasters of galaxies. The high-Machonumber shocks in young supernova remnants (SNRs)do not produce electron-ion temperature equilibration either. The heatingprocess in these collisionless shocks is not well understood, but the Coulombcollisions times are too long to provide the required heating.

编辑推荐

《等离子体天体物理学(第1部分):原理与实践(影印版)》主要是给等离子体天体物理领域的研究者提供参考之用，也同时会成为本专业以及空间物理、地球物理等专业的研究生感兴趣的读物。

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•   比较经典的一本，可以做入门用。价格也合适。