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High-Energy Radiation from Magnetized Neutron Stars

Neutron stars, the most extreme state of matter yet confirmed, are responsible for much of the high-energy radiation detected in the universe. Mèszàros provides a general overview of the physics of magnetized neutron stars, discusses in detail the radiation processes and transport properties relevant to the production and propagation of high-energy radiation in the outer layers of these objects, and reviews the observational properties and theoretical models of various types of neutron star sources.

546 pages | 177 figures | 6 x 9 | © 1992

Theoretical Astrophysics

Physical Sciences: Astronomy and Astrophysics, Physics and Astronomy

Table of Contents

1. Neutron Stars: An Overview
1.1. Formation
1.2. Neutron Star Physical Parameters
1.3. Structure of the Envelope and the Interior
1.4. Production of High-Energy Radiation from Magnetized Neutron Stars
1.5. Observations of High-Energy Radiation from Neutron Stars
2. Physics in a Strong Magnetic Field
2.1. Classical Motion of Charged Particles
2.2. The Onset of Quantum Effects in a Strong Magnetic Field
2.3. Quantum Treatment of the Electron in a Magnetic Field
2.4. Atomic Structure in a Strong Magnetic Field
2.5. Classical Electrodynamics in the Weak-Field Limit
2.6. Quantum Electrodynamics in Strong Fields
3. Magnetized Plasma Response Properties
3.1. Classical Wave Propagation in a Magnetized Plasma
3.2. Normal Modes of the Cold Magnetized Plasma
3.3. Quantum Mechanical Derivation of the Dielectric Tensor
3.4. Vacuum Polarizability Effects in Strongly Magnetized Plasmas
3.5. Thermal and Quantum Effects in the Nonrelativistic Limit
3.6. Validity of the Normal Mode Description
4. Magnetized Radiative Processes: Nonrelativistic Limit
4.1. The Radiation Process in an External Field
4.2. Electron Scattering in a Cold Plasma
4.3. Compton Scattering in a Hot Plasma
4.4. The Coulomb and Bremsstrahlung Processes
5. Relativistic Radiation Processes
5.1. Relativistic Cross Sections and Rates
5.2. Relativistic Redistribution Functions
5.3. Relativistic Wave Propagation
5.4. Synchrotron Radiation
5.5. Magnetic Pair Production and Annihilation
5.6. Other Magnetic Effects
6. Radiation Transport in Strongly Magnetized Plasmas
6.1. The Transport Equation
6.2. Approximate Solutions of the Polarized Transfer Equations
6.3. Numerical Treatments of the Transport Equation
6.4. Magnetic Comptonization Effects
6.5. Nonlinearities in Radiation Transport
7. Accreting X-Ray Pulsars
7.1. Observational Overview
7.2. Accretion Flow and Magnetosphere Models
7.3. The Accretion Column: Dynamics and Geometry
7.4. Negligible Radiation Pressure Models
7.5. Models with Radiation Pressure
7.6. Spectrum and Pulse Shape Models
8. Rotation-powered Pulsars
8.1. Observational Overview
8.2. The Standard Magnetic Dipole Model
8.3. Polar Cap Models
9. Gamma-Ray Bursters
9.1. Observational Overview
9.2. Gamma-Ray Burster Models and Energetics
9.3. Spectrum Formation in GRBs
10. Super-High-Energy Gamma-Ray Sources
10.1. Observational Overview
10.2. Models of VHE-UHE Gamma-Ray Sources
11. Evolution of Neutron Stars
11.1. Stellar Evolution of Neutron Star Systems
11.2. Thermal Evolution of Neutron Stars
11.3. Rotational Evolution of Neutron Stars
11.4. Magnetic Evolution of Neutron Stars
Appendix A: Relativistic Electron Wave Functions and Currents

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