Radiative Equilibrium of a Gaseous Nebula
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For radiatively ionized plasmas with densities exceeding about 102 electrons/cm3, the relaxation times of relevant physical processes are such that we can usually regard a given volume element as being in a steady state. If we can neglect mechanical effects, particularly energy gained or lost by compression or expansion, we can impose the condition of radiative equilibrium or energy balance. The amount of energy absorbed in each volume element then equals the amount emitted.
KeywordsMaxwellian Distribution Central Star Dielectronic Recombination Collisional Effect Radiative Equilibrium
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