1 introduction references 2 theory of mw emissions of solar flaring loo 2.1 observational characteristics of solar microwave emissions 2.1.1 intensity, polarization, and spectrum of mw emission 2.1.2 radiation transfer 2.1.3 thermal and nonthermal (nt) emission 2.2 gyrosynchrotron (gs) emission 2.2.1 emissivity and self-absorption coefficient 2.2.2 formation of gs spectrum 2.2.3 influence of magic field strength 2.2.4 influence of self-absorption 2.2.5 influence of high sma density: razin effect 2.2.6 razin effect and electron power-law index 2.2.7 sma density increase on the late decay phase.. 2.2.8 influence of sma inhomogeneity on gs spectrum 2.3 effects of electron pitch-angle anisotropy 2.3.1 parameters of numerical simulation 2.3.2 pitch-angle distributions of sinu type 2.3.3 effect of pitch-angle distribution shape: gaussian loss-cone 2.3.4 effect of pitch-angle distribution shape: beam-like distribution 2.3.5 discussion 2.4 trapping and transport effects 2.4.1 dependence on the ition of acceleration/injection site 2.4.2 spectral an polarization responses to specific electron distributions 2.4.3 diagnostic potential 2.5 effects of other parameters on gs emission 2.5.1 spectral shape 2.5.2 radio flux density 2.5.3 spectral index 2.5.4 turnover frequency 2.6 numerical codes for fast gs emission calculations references 3 observations and exnations of mw emissions in solar flaring loo 3.1 studies on spatially unresolvable observations 3.1.1 flattened spectra in solar radio bursts at cm and mm bands and dynamics of energetic electrons in flaring loo 3.1.2 dynamics of peak frequency in solar mw bursts: self-absorption and razin effect 3.1.3 optically thin emission, power-law distribution of flares, and occurrence rate of flares 3.2 spatial distribution of microwave brightness 3.2.1 nonthermal mw source at the top of extended flaring
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