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Protoplanets of Super-Earth sizes may get trapped in convergence zones forplanetary migration and form gas giants there. These growing planets undergoaccretion heating, which triggers a hot-trail effect that can reverse migrationdirections, increase eccentricities and prevent resonant captures (Chrenko etal. 2017). We study populations of embryos accreting pebbles using Fargo-Thorin2D hydrocode.  We find that embryos in a disk with high surface density ($\Sigma_0 =990\,{\rm g}\,{\rm cm}^{-2}$) undergo `unsuccessful' two-body encounters whichdo not lead to a merger. Only when a 3rd protoplanet arrives to the convergencezone, three-body encounters lead to mergers. For a low-viscosity disk ($\nu =5\times10^{13}\,{\rm cm}^2\,{\rm s}^{-1}$) a massive coorbital is a possibleoutcome, for which a pebble isolation develops and the coorbital is stabilised.For more massive protoplanets ($5\,M_\oplus$), the convergence radius islocated further out, in the ice-giant zone. After a series of encounters, thereis an evolution driven by a dynamical torque of a tadpole region, which issystematically repeated several times, until the coorbital configuration isdisrupted and planets merge. This may be a pathway how to solve the problemthat coorbitals often form in simulations but they are not observed in nature.  In contrast, the joint evolution of 120 low-mass protoplanets($0.1\,M_\oplus$) reveals completely different dynamics. The evolution is nolonger smooth, but rather a random walk. This is because the spiral arms,developed in the gas disk due to Lindblad resonances, overlap with each otherand affect not only a single protoplanet but several in the surroundings. Ourhydrodynamical simulations may have important implications for N-bodysimulations of planetary migration that use simplified torque prescriptions andare thus unable to capture protoplanet dynamics in its full glory.

Dynamics of multiple protoplanets embedded in gas/pebble disks and its dependence on $\Sigma$ and $\nu$ parameters