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E-raamat: Collisionless Plasmas in Astrophysics

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(Observatoire de Paris-Meudon, France), (Observatoire de Paris-Meudon, France), (Ecole Polytechnique, Palaiseau, France), (Observatoire de Grenoble, France), (Observatoire de Paris-Meudon, France)
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  • Ilmumisaeg: 10-Sep-2013
  • Kirjastus: Blackwell Verlag GmbH
  • Keel: eng
  • ISBN-13: 9783527656240
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Collisionless Plasmas in AstrophysicsSuurem pilt
  • Formaat: EPUB+DRM
  • Ilmumisaeg: 10-Sep-2013
  • Kirjastus: Blackwell Verlag GmbH
  • Keel: eng
  • ISBN-13: 9783527656240
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Astrophysicists Belmont Grappin, Mottez, Pantellini, and Pelletier present a basic textbook of plasma physics, and so encompass most classical topics of the discipline, such as turbulence, magnetic reconnection, linear waves, instability, and nonlinear effects. Their focus is on the collisionless limit and the consequences of the different modelings, fluid or kinetic in this case. Most of the examples are from the space physics of planetary magnetopsheres and solar wind. They cover plasma description and plasma models; the magnetized plasmas; collisional-collisionless; waves in plasmas; nonlinear effects, shocks, and turbulence; flow and particle acceleration processes; the transport and acceleration of cosmic rays; and the kinetic-fluid duality. Annotation ©2014 Book News, Inc., Portland, OR (booknews.com)

About the Authors XI
1 Introduction 1(46)
1.1 Goals of the Book
1(4)
1.2 Plasmas in Astrophysics
5(4)
1.2.1 Plasmas Are Ubiquitous
5(1)
1.2.2 The Magnetosphere of Stars
6(1)
1.2.3 Shock Waves
6(1)
1.2.4 Planetary Magnetospheres
7(2)
1.3 Upstream of Plasma Physics: Electromagnetic Fields and Waves
9(26)
1.3.1 Electromagnetic Fields
9(7)
1.3.2 Transverse and Longitudinal Electromagnetic Field
16(1)
1.3.3 Electromagnetic Fields in Vacuum
17(7)
1.3.4 Plane Waves in a Plasma
24(1)
1.3.5 Electromagnetic Components of Plane Plasma Waves
25(1)
1.3.6 Some General Properties of Plane Wave Polarization and Dispersion
26(1)
1.3.7 Electrostatic Waves
27(1)
1.3.8 Wave Packets and Group Velocity
28(1)
1.3.9 Propagation of Plane Waves in a Weakly Inhomogeneous Medium
28(2)
1.3.10 Useful Approximations of the Maxwell Equations in Plasma Physics
30(5)
1.4 Upstream of Plasma Physics: The Motion of Charged Particles
35(12)
1.4.1 The Motion of the Guiding Center
35(4)
1.4.2 Adiabatic Invariants
39(3)
1.4.3 The Motion of a Particle in a Wave
42(5)
2 Plasma Descriptions and Plasma Models 47(30)
2.1 Distribution Function and Moments
47(11)
2.1.1 From Individual Particles to Kinetic Description
47(3)
2.1.2 Kinetic Description and First Order Moments
50(3)
2.1.3 Higher-Order Moments
53(1)
2.1.4 Moments for a Mixture of Populations
54(1)
2.1.5 Nontrivial Generalization of the Fluid Concepts
55(2)
2.1.6 Fluid vs. Kinetic Description: An Example
57(1)
2.2 From Kinetic to Fluid Equations
58(9)
2.2.1 Moment Equations
58(4)
2.2.2 Lagrangian Form of the Moment Equations
62(1)
2.2.3 Fluid Equations: Necessity of a Closure Equation
63(2)
2.2.4 Collisional Limit: Fluid Dynamics and Thermodynamics
65(2)
2.3 Numerical Methods
67(7)
2.3.1 Vlasov Codes
67(2)
2.3.2 Particle in Cell Codes (PIC)
69(4)
2.3.3 Perturbative PIC Codes
73(1)
2.4 Fluid Codes
74(1)
2.5 Hybrid Codes
75(2)
3 The Magnetized Plasmas 77(28)
3.1 Ideal MHD
77(5)
3.1.1 The Ideal MHD System
77(2)
3.1.2 The Ideal Ohm's Law
79(3)
3.2 Establishing the MHD Model
82(6)
3.2.1 Large-Scale Conditions of Validity
85(1)
3.2.2 Departures from MHD: Multi-Fluid and Kinetic Effects
86(2)
3.3 Dimensional Analysis and Plasma Characteristic Scales
88(17)
3.3.1 Dimensional Analysis: The General Methods
88(4)
3.3.2 Temporal and Spatial Scales, Adimensional Numbers
92(10)
3.3.3 Dispersive and Dissipative Effects
102(1)
3.3.4 Physical Importance of the Dimensionless Parameters
103(2)
4 Collisional-Collisionless 105(30)
4.1 Notion of Collisions in Plasma Physics
105(14)
4.1.1 Coulomb Interaction: A Long Range Interaction
105(4)
4.1.2 Mean Free Path
109(4)
4.1.3 The Debye Length and the Notion of Debye "Screening"
113(2)
4.1.4 Knudsen Number
115(2)
4.1.5 Plasma Regimes
117(2)
4.2 Notion of Dissipation
119(16)
4.2.1 Transfers of Energy and Dissipation
119(1)
4.2.2 The Concept of Dissipation in Collisional Fluids
120(3)
4.2.3 Reversibility
123(2)
4.2.4 Irreversibility and Damping
125(2)
4.2.5 The Notion of Reversibility Depends on the Description
127(5)
4.2.6 Entropy
132(3)
5 Waves in Plasmas 135(64)
5.1 MHD Waves
136(4)
5.1.1 Polarization of the MHD Waves
137(2)
5.1.2 Application: Alfven and MHD Waves in the Earth's Magnetosphere
139(1)
5.2 Transport Induced by Waves
140(6)
5.2.1 Alfven Wave Pressure
141(5)
5.3 High-Frequency Waves
146(8)
5.3.1 Cold Plasma Model
146(2)
5.3.2 Parallel Propagation
148(2)
5.3.3 Perpendicular Propagation: Ordinary and Extraordinary Waves
150(1)
5.3.4 Application: Plasma Cut-offs and Limits to the Radio Astronomy
151(1)
5.3.5 Application: The Dispersion of Radio Waves from Pulsars
152(1)
5.3.6 Application: Faraday Rotation in the Interstellar Medium
153(1)
5.4 Whistler Mode
154(4)
5.5 Collisional Damping in Fluid Theories
158(10)
5.5.1 Dissipative Effects and Entropy
158(3)
5.5.2 Dissipation and Collisions
161(2)
5.5.3 Strongly Collisional Systems
163(1)
5.5.4 Heat Conduction: From Collisional to Collisionless
164(3)
5.5.5 The Thermoelectric Field: Another Consequence of Collisions between Ions and Electrons
167(1)
5.6 Collisionless Damping
168(25)
5.6.1 Number of Eigenmodes: Fluid vs. Kinetic
168(1)
5.6.2 A Simple Example: The Langmuir Wave, from Fluid to Kinetic
169(1)
5.6.3 Fluid Treatment of the Langmuir Wave: Choice of a Closure
170(6)
5.6.4 Kinetic Treatment of the Langmuir Wave: Landau Damping
176(16)
5.6.5 Other Types of Kinetic Damping
192(1)
5.7 Instabilities
193(6)
5.7.1 Real Space Instabilities: Fluid Treatment
193(1)
5.7.2 Velocity Space Instabilities: Kinetic Treatment
193(1)
5.7.3 Weak Kinetic Effects
194(2)
5.7.4 An Example: The Two-Stream Instability
196(3)
6 Nonlinear Effects, Shocks, and Turbulence 199(76)
6.1 Collisionless Shocks and Discontinuities
199(14)
6.1.1 Nonlinear Propagation, Discontinuities, Jumps
199(6)
6.1.2 Shocks and Other Discontinuities in a Magnetized Plasma
205(3)
6.1.3 The Unmagnetized Shock Wave
208(1)
6.1.4 A Particular Case: The Tangential Discontinuity
208(3)
6.1.5 Example: The Terrestrial Bow Shock, the Foreshocks
211(2)
6.2 Turbulence (Mainly MHD)
213(40)
6.2.1 Hydrodynamics: Equations, Shocks
216(4)
6.2.2 Hydrodynamics: 3D Incompressible Turbulence
220(5)
6.2.3 MHD Turbulence - Introduction
225(5)
6.2.4 Weak Isotropic (IK) Regime
230(5)
6.2.5 Anisotropic Regimes
235(15)
6.2.6 Discussion
250(3)
6.3 Nonlinear Kinetic Physics
253(22)
6.3.1 Nonlinear Electrostatic Waves
254(1)
6.3.2 Particle Trapping
255(8)
6.3.3 The Nonlinear Interaction of Many Electrostatic Waves of Low Amplitude
263(2)
6.3.4 Quasi-Linear Theory
265(4)
6.3.5 Trapping versus Quasi-Linear Diffusion
269(6)
7 Flow and Particle Acceleration Processes 275(44)
7.1 Flow Acceleration and Heating in a Collisional Fluid
275(19)
7.1.1 Basic Equations
275(4)
7.1.2 Expressions for the Polytropic Fluids
279(2)
7.1.3 Bernoulli's Principle
281(1)
7.1.4 Venturi Effect
281(2)
7.1.5 De Laval Nozzle
283(1)
7.1.6 Stellar Winds
284(7)
7.1.7 Possible Routes to Turbulence in Stellar Winds
291(2)
7.1.8 Accretion
293(1)
7.2 Magnetic Reconnection
294(11)
7.2.1 Conservation of Connections vs. Reconnection
294(2)
7.2.2 Departure from the Ideal Ohm's Law: Microscopic Mechanisms and Macroscopic Consequences
296(1)
7.2.3 Flow Acceleration by Reconnection
297(5)
7.2.4 Tearing Instability
302(2)
7.2.5 3D Reconnection
304(1)
7.3 Kinetic Acceleration Processes in Magnetospheres
305(14)
7.3.1 Substorms and Auroras in the Earth's Magnetosphere
305(2)
7.3.2 Fermi Acceleration in the Magnetosphere
307(1)
7.3.3 Acceleration by a Forced Current Forced along Convergent Magnetic Field Lines
307(4)
7.3.4 Acceleration by an Electric Current Forced by a Wave
311(1)
7.3.5 Acceleration by an Alfven Wave (NonMHD) Parallel Electric Field
312(3)
7.3.6 Resonant Acceleration by a Wave
315(1)
7.3.7 Acceleration by a Wave of Short Length
316(1)
7.3.8 Application: Acceleration in the Earth's Magnetosphere
317(2)
8 Transport and Acceleration of Cosmic Rays 319(38)
8.1 The Problem of Transport
320(16)
8.1.1 The Magnetic Field: Obstruction to Transport
320(2)
8.1.2 Magnetic Irregularities: Transport Agent
322(5)
8.1.3 Other Diffusion Coefficients
327(3)
8.1.4 Transport Equation of Cosmic Rays
330(4)
8.1.5 Distribution of Suprathermal Particles Crossing a Shock
334(2)
8.1.6 From Transport to Acceleration
336(1)
8.2 Fermi Acceleration of Cosmic Rays
336(21)
8.2.1 The Basic Fermi Process
338(8)
8.2.2 Fermi Process at a Nonrelativistic Shock
346(4)
8.2.3 Astrophysical Application: Cosmic Rays and Supernovae
350(1)
8.2.4 Astrophysical Application: Synchrotron Sources
351(2)
8.2.5 Generation of Magnetic Turbulence
353(1)
8.2.6 Why Are Fermi Processes Favored at Shocks?
354(1)
8.2.7 What about the Relativistic Regime of Fermi Acceleration?
355(2)
9 The Kinetic-Fluid Duality 357(26)
9.1 Toy Models
357(11)
9.1.1 Small Amplitude Ballistic Fluctuations
358(3)
9.1.2 Large-Amplitude Ballistic Fluctuations
361(5)
9.1.3 Quasi-Fluid Behavior of a Collisionless Plasma: Launching a 2D Plasma Bullet
366(2)
9.2 Solar and Stellar Wind Expansion
368(15)
9.2.1 A Simple Noncollisional Wind
368(2)
9.2.2 More Sophisticated Noncollisional Wind Models
370(1)
9.2.3 Charge Neutralizing Field for a Plasma in a Gravitational Field
371(3)
9.2.4 Qualitative Radial Profile of the Total Proton Potential
374(2)
9.2.5 Charge Neutralizing Electric Field and Dreicer Field
376(1)
9.2.6 Electric Field Intensity at the Sonic Radius rs
377(1)
9.2.7 Effective Closure for the Solar Wind
377(6)
Appendix 383(12)
A.1 Notation
383(2)
A.1.1 Vectors and Tensors
383(1)
A.1.2 Derivatives
383(1)
A.1.3 List of Notation
384(1)
A.2 Asymptotic Expansions and Adiabatic Invariants
385(8)
A.2.1 Multiscale Expansion
385(3)
A.2.2 The Adiabatic Invariants
388(2)
A.2.3 Derivation of the Guiding Center Equations
390(3)
A.3 Fokker-Planck Equation, First Order Term
393(2)
References 395(10)
Index 405
Gerard Belmont works as a "Directeur de Recherches" at the French CNRS for twenty years. He is a specialist of collisionless media, and their description through kinetic and fluid theories.

Roland Grappin is Astronomer at the Paris Observatory since 1979. His scientific activity covers turbulence in fluids and plasmas, dynamics of the solar wind, corona and transition region.

Fabrice Mottez is a scientist at the Paris Observatory. He has devoted his career to collisionless space plasmas, the terrestrial and Jovian magnetospheres, fundamental plasma physics, and numerical simulation.

Filippo Pantellini is a scientist at the Paris Observatory. His main research fields cover the theoretical and numerical investigation of collisionless and weakly collisional space plasmas, with a particular interest for the solar wind and the solar corona.

Guy Pelletier is a professor at the University Joseph Fourier in Grenoble. He founded the theoretical group of the Laboratory for Astrophysics. He accessed to all the levels of professorship and got the status of Emeritus Professor in 2009
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