Spontaneous Current Sheets in Magnetic Fields

Name: Spontaneous Current Sheets in Magnetic Fields | With Applications to Stellar X-rays
Brand: OUP eBook
Price: 115.99 EUR
Availability: OnlineOnly

With Applications to Stellar X-rays

Eugene N. Parker(Autor*in)

OUP eBook (Verlag)

Erschienen am 21. Juli 1994

435 Seiten

E-Book

PDF mit Adobe-DRM

Systemvoraussetzungen

978-0-19-536085-1 (ISBN)

115,99 €inkl. 7% MwSt.

Systemvoraussetzungen

für PDF mit Adobe-DRM

E-Book Einzellizenz

Als Download verfügbar

Beschreibung

Weitere Details

Weitere Ausgaben

Person

Inhalt

Intro
Contents
1 INTRODUCTION
1.1 The General Picture
1.2 Activity of Stars and Galaxies
1.3 The Nature of Active Magnetic Fields
1.4 Rapid Dissipation
1.5 The Magnetostatic Theorem
1.6 Continuous Magnetostatic Fields
1.7 Perturbations of a Continuous Field
1.8 Tangential Discontinuities
1.9 The Optical Analogy
1.10 General Discussion
1.11 Hydrodynamic Turbulence
2 THE FIELD EQUATIONS
2.1 Appropriate Field Concepts
2.1.1 Momentum and Energy of the Particles
2.1.2 Electromagnetic Momentum and Energy
2.2 The MHD Limit
2.2.1 Statistical Averages
2.2.2 Electromagnetics of a Noninsulating Fluid
2.2.3 Electromagnetics of a Weakly Insulating Fluid
2.2.4 Alternative Formulations
2.3 The MHD Equations in a Tenuous Plasma
2.4 Deviations from MHD
2.4.1 Parallel Electric Field
2.4.2 Surfaces of Discontinuity
2.4.3 Anomalous Resistivity
2.4.4 Onset of Anomalous Resistivity and Electric Double Layers
3 INVARIANCE, DEGENERACY, AND CONTINUOUS SOLUTIONS
3.1 Magnetostatic Equilibrium Equations
3.2 Field Configurations
3.3 Basic Field Configuration
3.4 Characteristics and Discontinuities
3.5 Unlimited Winding
3.6 Action at a Distance
4 FORMAL STRUCTURE OF THE MAGNETOSTATIC EQUATIONS
4.1 Introduction
4.2 Continuous Solutions
4.3 Invariant Fields
4.4 Nearly Invariant Fields
4.5 Infinitesimal Perturbation to a Force-Free Field
4.6 Integral Constraints
4.7 Further Integral Constraints
4.8 Infinitesimal Perturbation Including Fluid Pressure
4.9 Physical Basis for Tangential Discontinuities
4.10 Discontinuities and Dynamical Nonequilibrium
4.11 Hamiltonian Formulation of the Magnetostatic Field
4.11.1 Reformulation of Hamiltonian Representation
4.11.2 Destruction of Flux Surfaces
5 DIRECT INTEGRATION OF EQUILIBRIUM EQUATIONS
5.1 Description of the Field
5.2 The Equilibrium Equations for a Force-Free Field
5.3 Topology of Field Lines
5.4 The Primitive Torsional Field
5.4.1 Elementary Integration
5.4.2 Asymptotic Solution
5.5 Continuous Solutions
5.5.1 Solution for Primitive Force-Free Field
5.5.2 The Field Topology
Appendix: Field Lines in a Canted Field
6 EXAMPLES OF FIELD DISCONTINUITIES
6.1 Introduction
6.2 Compression of a Primitive Force-Free Field
6.3 Tangential Discontinuities in Two Dimensions
6.4 Free Energy of a Discontinuity
6.5 The Y-Type Neutral Point in a Potential Field
6.6 Free Energy Above a Plane Boundary
6.7 Free Energy of an Extended Neutral Point
6.8 The Creation of X-Type Neutral Points
6.9 Direct Numerical Simulation
6.10 Discontinuity Through Instability
6.11 Discontinuities Between Twisted Flux Bundles
6.12 Physical Construction of Continuous Fields
6.13 Time-Dependent Fields
7 THE OPTICAL ANALOGY
7.1 The Basic Construction
7.2 Special Cases
7.3 The Field Rotation Effect
7.4 Refraction Around a Maximum
7.4.1 General Parabolic Maximum
7.4.2 Gaussian Maximum
7.5 Non-Euclidean Surfaces
7.6 Refraction in a Slab and Field Line Topology
7.7 Relative Motion of Index of Refraction
7.8 Bifurcation of Fields
7.9 Gaps and Various Discontinuities
7.10 Topology Around a Field Maximum
7.11 Displacement of Individual Flux Bundles
8 TOPOLOGY OF TANGENTIAL DISCONTINUITIES
8.1 Conservation of Discontinuities
8.2 Fluid Pressure
8.3 The Primitive Discontinuity
8.4 Topology Around Neutral Points
8.5 General Form of Discontinuities
8.6 Field Structure Around Intersecting Discontinuities
8.6.1 Magnetostatic Field in a Vertex
8.6.2 Compatibility of Sectors
8.7 Discontinuities Around Displaced Flux Bundles
9 FLUID MOTIONS
9.1 Collision of Separate Regions
9.1.1 Inviscid Fluid
9.1.2 Viscous Fluid
9.1.3 Viscosity and Resistivity
9.2 High Speed Sheets
9.3 Dynamical Model
9.4 Hydrodynamic Model of High Speed Sheet
9.5 Displaced Flux Bundles
10 EFFECTS OF RESISTIVITY
10.1 Diffusion of a Current Sheet
10.2 Dissipation with Continuing Shear
10.3 Dynamical Dissipation
10.3.1 Basic Concepts
10.3.2 Basic Relations
10.3.3 Limits of Reconnection
10.3.4 Theoretical Developments
10.3.5 Tearing Instability
10.3.6 The Complementary Approach
10.3.7 The Third Dimension
10.4 Nonuniform Resistivity
10.4.1 Quasi-static Plane Current Sheet
10.4.2 Alfven Transit Time Effects
10.4.3 Upward Extension of Current Sheet Thickness
10.4.4 Nonuniform Current Sheets
10.5 Changes in Field Topology
11 SOLAR X-RAY EMISSION
11.1 The Origin of X-Ray Astronomy
11.1.1 Theoretical Considerations
11.2 Conditions in the X-Ray Corona
11.2.1 Variability in the X-Ray Corona
11.3 General Considerations
11.3.1 Detailed Modeling of Coronal Loops
11.4 Toward a Theory of Coronal Heating
11.4.1 Waves in the Corona
11.4.2 Wave Dissipation
11.4.3 The Wave Dilemma
11.4.4 Quasi-static Fields
11.4.5 Energy Input to Quasi-static Fields
11.4.6 Dissipation of Quasi-static Fields
11.4.7 Energy of the Basic Nanoflare
11.4.8 Physical Properties of the Basic Nanoflare
11.4.9 Variation Along a Coronal Loop
11.5 Observational Tests
12 UNIVERSAL NANOFLARES
12.1 General Considerations
12.2 The Solar Flare
12.2.1 Basic Nature of the Flare Release
12.2.2 Nanoflare Size
12.2.3 Preflare Deformation
12.2.4 Flare Size Distribution
12.2.5 Internal Dynamics
12.3 The Geomagnetic Field
12.3.1 Aurorae
12.4 Diverse Settings
12.5 Cosmic Rays and Galactic Halos
12.6 Observational and Experimental Studies of Nanoflaring
References
Index
A
B
C
D
E
F
G
H
I
K
L
M
N
O
P
R
S
T
U
V
X

Systemvoraussetzungen

Als PDF speichern Als Link merken