Radiative Processes in AstrophysicsRadiative Processes in Astrophysics: This clear, straightforward, and fundamental introduction is designed to present-from a physicist's point of view-radiation processes and their applications to astrophysical phenomena and space science. It covers such topics as radiative transfer theory, relativistic covariance and kinematics, bremsstrahlung radiation, synchrotron radiation, Compton scattering, some plasma effects, and radiative transitions in atoms. Discussion begins with first principles, physically motivating and deriving all results rather than merely presenting finished formulae. However, a reasonably good physics background (introductory quantum mechanics, intermediate electromagnetic theory, special relativity, and some statistical mechanics) is required. Much of this prerequisite material is provided by brief reviews, making the book a self-contained reference for workers in the field as well as the ideal text for senior or first-year graduate students of astronomy, astrophysics, and related physics courses. Radiative Processes in Astrophysics also contains about 75 problems, with solutions, illustrating applications of the material and methods for calculating results. This important and integral section emphasizes physical intuition by presenting important results that are used throughout the main text; it is here that most of the practical astrophysical applications become apparent. |
From inside the book
Results 1-5 of 20
Page xiv
... Ionization 259 Thermal Equilibrium: Boltzmann Population of Levels 259 The Saha Equation 260 PROBLEMS 263 REFERENCES 266 CHAPTER 10 RADIATIVE TRANSITIONS 267 10.1 10.2 10.3 10.4 10.5 Semi-Classical Theory of Radiative Transitions 267 ...
... Ionization 259 Thermal Equilibrium: Boltzmann Population of Levels 259 The Saha Equation 260 PROBLEMS 263 REFERENCES 266 CHAPTER 10 RADIATIVE TRANSITIONS 267 10.1 10.2 10.3 10.4 10.5 Semi-Classical Theory of Radiative Transitions 267 ...
Page 46
You have reached your viewing limit for this book.
You have reached your viewing limit for this book.
Page 47
You have reached your viewing limit for this book.
You have reached your viewing limit for this book.
Page 104
You have reached your viewing limit for this book.
You have reached your viewing limit for this book.
Page 165
You have reached your viewing limit for this book.
You have reached your viewing limit for this book.
Other editions - View all
Common terms and phrases
absorption coefficient angular momentum approximation assume atomic average blackbody bremsstrahlung charge classical components Compton scattering configuration constant cosé cross section defined density depends derived dipole direction distribution Doppler effect Einstein electric field electromagnetic electron emitted energy equilibrium expression factor Figure flux formula four-vector four-velocity given gives hydrogen integral inverse Compton ionization isotropic levels Lorentz invariant Lorentz transformation magnetic field Maxwell's equations medium molecule nonrelativistic Note observer obtain optical depth optically thick orbital oscillator parameters parity particle photon plane plasma polarization potential Problem propagation pulse quantities quantum number radiation field radiation reaction radiative relation relativistic rest frame result rotational scalar scattering selection rules simply solid angle source function specific intensity spectra spectrum spin Stokes parameters temperature tensor thermal tion transition unit volume values vector velocity wave function