  We study the influence of kinetic-scale Alfv\'enic turbulence on the
generation of plasma radio emission in the solar coronal regions where the
plasma/magnetic pressure ratio $\beta $ is smaller than the electron/ion mass
ratio $m_{e}/m_{i}$. The present study is motivated by the phenomenon of solar
type I radio storms associated with the strong magnetic field of active
regions. 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 I
bursts. At present, there is no generally accepted theory explaining such high
brightness temperatures and some other properties of the type I storms. We
propose the model with the imbalanced turbulence of kinetic-scale Alfv\'en
waves producing an asymmetric quasilinear plateau on the upward half of the
electron velocity distribution. The Landau damping of resonant Langmuir waves
is suppressed and their amplitudes grow spontaneously above the thermal level.
The estimated saturation level of Langmuir waves is high enough to generate
observed type I radio emission at the fundamental plasma frequency. Harmonic
emission does not appear in our model because the backward-propagating Langmuir
waves undergo a strong Landau damping. Our model predicts $100\%$ polarization
in the sense of the ordinary (o-) mode of type I emission.
