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Due to the gravitational influence of density fluctuations driven bymagneto-rotational instability in the gas disk, planetesimals and protoplanetsundergo diffusive radial migration as well as changes in other orbitalproperties. The magnitude of the effect on particle orbits can have importantconsequences for planet formation scenarios. We use the local-shearing-boxapproximation to simulate an ideal, isothermal, magnetized gas disk withvertical density stratification and simultaneously evolve numerous masslessparticles moving under the gravitational field of the gas and the host star. Wemeasure the evolution of the particle orbital properties, including meanradius, eccentricity, inclination, and velocity dispersion, and its dependenceon the disk properties and the particle initial conditions. Although theresults converge with resolution for fixed box dimensions, we find the responseof the particles to the gravity of the turbulent gas correlates with thehorizontal box size, up to 16 disk scale heights. This correlation indicatesthat caution should be exercised when interpreting local-shearing-box modelsinvolving gravitational physics of magneto-rotational turbulence. Based onheuristic arguments, nevertheless, the criterion L_h / R ~ O(1), where L_h isthe horizontal box size and R is the distance to the host star, is proposed topossibly circumvent this conundrum. If this criterion holds, we can stillconclude that magneto-rotational turbulence seems likely to be ineffective atdriving either diffusive migration or collisional erosion under mostcircumstances.

Planetesimal and Protoplanet Dynamics in a Turbulent Protoplanetary Disk: Ideal Stratified Disks