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We present high resolution 3-D simulations of the planet-disc interactionusing smoothed particle hydrodynamics, to investigate the possibility ofdriving eccentricity growth by this mechanism. For models with a given discviscosity (\alpha = 0.01), we find that for small planet masses (a few Jupitermasses) and canonical surface densities, no significant eccentricity growth isseen over the duration of our simulations. This contrasts with the limitingcase of large planet mass (over twenty Jupiter masses) and extremely highsurface densities, where we find eccentricity growth in agreement withpreviously published results. We identify the cause of this as being athreshold surface density for a given planet mass below which eccentricitygrowth cannot be excited by this method. Further, the radial profile of thedisc surface density is found to have a stronger effect on eccentricity growththan previously acknowledged, implying that care must be taken when contrastingresults from different disc models. We discuss the implication of this resultfor real planets embedded in gaseous discs, and suggest that the disc-planetinteraction does not contribute significantly to observed exoplaneteccentricities.

A limit on eccentricity growth from global 3-D simulations of disc-planet interactions