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Terrestrial planets are commonly observed to orbit M dwarfs with close-intrajectories. In this work, we extensively perform N-body simulations ofplanetesimal accretion with three models of in-situ, inward migration andreversed migration to explore terrestrial formation in tightly compact systemsof M dwarfs. In the simulations, the solid disks are assumed to be 0.01\% ofthe masses of host stars and spread from 0.01 to 0.5 AU with the surfacedensity profile scaling with $r^{-k}$ according to the observations. Ourresults show that in-situ scenario may produce $7.77^{+3.23}_{-3.77}$terrestrial planets with an average mass of $1.23^{+4.01}_{-0.93} \ M_{\oplus}$around M dwarfs. The number of planets tends to increase as the disk slope issteeper or with a larger stellar mass. Moreover, we show that$2.55^{+1.45}_{-1.55}$ planets with mass of $3.76^{+8.77}_{-3.46} \ M_{\oplus}$are formed in the systems via inward migration, while $2.85^{+1.15}_{-0.85}$planets with $3.01^{+13.77}_{-2.71} \ M_{\oplus}$ are yielded under reversedmigration. Migration scenarios can also deliver plentiful water from theexterior of ice line to the interior due to more efficient accretion. Thesimulation outcomes of reversed migration model produce the best matching withobservations, being suggestive of a likely mechanism for planetary formationaround M dwarfs.

The Terrestrial Planet Formation around M Dwarfs: In-situ, Inward Migration or Reversed Migration