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We propose a pebble-driven core accretion scenario to explain the formationof giant planets around the late-M dwarfs of $M_{\star}{=}0.1{-}0.2 \M_{\odot}$. In order to explore the optimal disk conditions for giant planet,we perform N-body simulations to investigate the growth and dynamical evolutionof both single and multiple protoplanets in the disks with both inner viscouslyheated and outer stellar irradiated regions. The initial masses of theprotoplanets are either assumed to be equal to $0.01 \ M_{\oplus}$ orcalculated based on the formula derived from streaming instability simulations.Our findings indicate that massive planets are more likely to form in diskswith longer lifetimes, higher solid masses, moderate to high levels of diskturbulence, and larger initial masses of protoplanets. In the singleprotoplanet growth cases, the highest planet core mass that can be reached isgenerally lower than the threshold necessary to trigger rapid gas accretion,which impedes the formation of giant planets. Nonetheless, in multi-protoplanetcases, the cores can exceed the pebble isolation mass barrier aided by frequentplanet-planet collisions. This consequently speeds up their gas accretion andpromotes giant planet formation, making the optimal parameter space to growgiant planets substantially wider. Taken together, our results suggest thateven around very low-mass stellar hosts, the giant planets with orbital periodsof ${\lesssim}100$ days are still likely to form when lunar-mass protoplanetsfirst emerge from planetesimal accretion and then grow rapidly by a combinationof pebble accretion and planet-planet collisions in disks with a high supply ofpebble reservoir ${>}50 \ M_{\oplus}$ and turbulent level of $\alpha_{\rm t}{\sim} 10^{-3}{-}10^{-2}$.

Forming Giant Planets Around Late-M Dwarfs: Pebble Accretion and Planet-Planet Collision