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We study the influence of kinetic-scale Alfv\'enic turbulence on thegeneration of plasma radio emission in the solar coronal regions where theplasma/magnetic pressure ratio $\beta $ is smaller than the electron/ion massratio $m_{e}/m_{i}$. The present study is motivated by the phenomenon of solartype I radio storms associated with the strong magnetic field of activeregions. The measured brightness temperature of the type I storms can be up to$10^{10}$ K for continuum emission, and can exceed $10^{11}$ K for type Ibursts. At present, there is no generally accepted theory explaining such highbrightness temperatures and some other properties of the type I storms. Wepropose the model with the imbalanced turbulence of kinetic-scale Alfv\'enwaves producing an asymmetric quasilinear plateau on the upward half of theelectron velocity distribution. The Landau damping of resonant Langmuir wavesis suppressed and their amplitudes grow spontaneously above the thermal level.The estimated saturation level of Langmuir waves is high enough to generateobserved type I radio emission at the fundamental plasma frequency. Harmonicemission does not appear in our model because the backward-propagating Langmuirwaves undergo a strong Landau damping. Our model predicts $100\%$ polarizationin the sense of the ordinary (o-) mode of type I emission.

Solar plasma radio emission in the presence of imbalanced turbulence of kinetic-scale Alfv\'en waves