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Other effects like exciton hopping [11, 12] and non-radiative radiation via defects [13] can change the wavelength-dependent quantum efficiencies and, thus, the final emission spectrum.
Besides the adiabatic model neglecting radiative loss, two radiation models are used in simulation: one is the optically thin model considering only radiation emission and the other is the statistical narrow band model considering both radiation emission and absorption.
These heat transfer coefficients enabled the separation of the heat transfer into convective and radiative components, with radiation being the dominant transfer mechanism for blackened loads.
The effects of radiative loss and radiation absorption on large-scale spherical flame propagation are quantified through comparison among results predicted by these three models.
The statistical and discretization errors of the computed radiative heat flux and radiation source term are isolated and quantified.
Using the Rosseland approximation for radiation, the radiative heat flux is simplified as: q r = - 4 σ * 3 k * ∂ T 4 ∂ y, (6).
Using the Rosseland approximation for radiation, the radiative heat flux is {q}_{mathrm{r}}=frac{-4{sigma}_{mathrm{sB}}}{3{m}_0}lefrac{partialial {T}^4}{partial z}right), (9).
Comparisons of adiabatic and radiative calculations show that radiation can have a significant effect on the width and structure of partially premixed flames, as well as on the levels of NO produced.
The dimensionless incident radiation and net radiative heat flux are obtained using the DRESOR method.
The top-down mechanism originates in the stratosphere where UV radiation modulates local radiative heating at the tropical stratopause.
We also compute the rates of emission of radiation and the radiative efficiency, and discuss comparisons with observations.
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