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We use analytic estimates and numerical simulations of test particlesinteracting with magnetohydrodynamic (MHD) turbulence to show that subsonic MHDturbulence produces efficient second-order Fermi acceleration of relativisticparticles. This acceleration is not well-described by standard quasi-lineartheory but is a consequence of resonance broadening of wave-particleinteractions in MHD turbulence. We provide momentum diffusion coefficients thatcan be used for astrophysical and heliospheric applications and discuss theimplications of our results for accretion flows onto black holes. Inparticular, we show that particle acceleration by subsonic turbulence inradiatively inefficient accretion flows can produce a non-thermal tail in theelectron distribution function that is likely important for modeling andinterpreting the emission from low luminosity systems such as Sgr A* and M87.

Acceleration of Relativistic Electrons by MHD Turbulence: Implications for Non-thermal Emission from Black Hole Accretion Disks