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(Abridged).We present the results of MHD simulations of low mass protoplanetsinteracting with turbulent disks. We calculate the orbital evolution of`planetesimals' and protoplanets with masses in the range 0 < m_p < 30 M_Earth.Planetesimals and protoplanets undergo stochastic migration due to interactionwith turbulent density fluctuations. Over run times of ~ 150 planet orbits,stochastic migration dominates over type I migration for many models. Fourieranalysis of the torques experienced by planets indicates that the torquefluctuations contain components with significant power whose time scales ofvariation are similar to the simulation run times. These low frequencyfluctuations partly explain the dominance of stochastic torques, and mayprovide a powerful means of counteracting the type I migration of some planetsin turbulent disks. Turbulence is a source of eccentricity driving.Planetesimals attained eccentricities in the range 0.02 < e < 0.14, m_p=1M_Earth planets attained eccentricities 0.02 < e < 0.08, and m_p=10 M_Earthprotoplanets reached 0.02 < e < 0.03. This is in basic agreement with a modelin which turbulence drives e-growth, and interaction with disk material atcoorbital Lindblad resonances causes e-damping. These results are significantfor planet formation. Stochastic migration may prevent some planet coresmigrating into their star via type I before becoming gas giants. The growth ofplanetary cores may be enhanced by preventing isolation. Eccentricityexcitation by turbulence, however, may reduce growth rates of planetary coresduring the runaway and oligarchic growth stages, and cause collisions betweenplanetesimals to become destructive.

On the orbital evolution of low mass protoplanets in turbulent, magnetised disks