Opacity pp 263-286 | Cite as

Continuum Transitions

Part of the Astrophysics and Space Science Library book series (ASSL, volume 402)


At low densities and low temperatures most of the cross sections discussed in Chap. 5 can be applied directly to opacity calculations. In all other cases we also must pay attention to shielding by free electrons, Fermi–Dirac statistics including the Pauli exclusion principle, collective effects of free electrons, random motion (temperature) of the absorbing and scattering particles, and (for computational convenience) statistical distributions of the states of excitation. The effects of these processes on bound–bound transitions (including resonance scattering) are discussed in Chap. 7; here we consider only the processes leading to the continuous opacity. Absorption and scattering coefficients are directly proportional to the occupation of the initial state as determined by the equation of state, e.g., Eq. (4.8). We also include here the effects of size distribution of grains and droplets on opacity.


Free Absorption Pauli Exclusion Principle Scatter Phase Shift Inverse Bremsstrahlung Maxwell Velocity Distribution 
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