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The torques exerted by a locally isothermal disk on an embedded planet leadto rapid inward migration. Recent work has shown that modeling thethermodynamics without the assumption of local isothermality reveals regionswhere the net torque on an embedded planet is positive, leading to outwardmigration of the planet. When a region with negative torque lies directlyexterior to this, planets in the inner region migrate outwards and planets inthe outer region migrate inwards, converging where the torque is zero. Weincorporate the torques from an evolving non-isothermal disk into an N-bodysimulation to examine the behavior of planets or planetary embryos interactingin the convergence zone. We find that mutual interactions do not eject objectsfrom the convergence zone. Small numbers of objects in a laminar disk settleinto near resonant orbits that remain stable over the 10 Myr periods that weexamine. However, either or both increasing the number of planets or includinga correlated, stochastic force to represent turbulence drives orbit crossingsand mergers in the convergence zone. These processes can build gas giant coreswith masses of order ten Earth masses from sub-Earth mass embryos in 2-3 Myr.

Orbital migration of interacting low-mass planets in evolutionary radiative turbulent models