The origin of the energetic particles associated with solar flares is a challenge to solar plasma theory. In this paper, we investigate the feature of stochastic acceleration of electrons by lower hybrid (LH) turbulence, which is a possible mechanism for the energization of relativistic electrons. The transport and acceleration parameters are studied with the Fokker-Planck coefficients Dμμ, Dμp, and Dpp, obtained from the quasi-linear method under the test particle assumption. Using the analytic expressions of the diffusion coefficients, we obtain the aspects of electron acceleration by LH turbulence, such as the acceleration and scattering timescales. The results show that the acceleration time of an original thermal electron over 20 keV is less than 1 s, which is required by hard X-ray observations during impulsive flares. However, the isotropy of the pitch-angle distribution cannot be maintained, and high-energy (~100 MeV) acceleration is inefficient. Some results of different plasma cases are compared, which are helpful in the understanding of particle acceleration in solar flares.
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