Two-dimensional simulations of the flyby of an M dwarf system through a protoplanetary disk. The total mass of the protoplanetary disk is 0.12 M_⊙, with a 1 M_⊙ central star. Four sets of parameters are considered as initial conditions: (a) disk radius R_d = 150 au, mass of the M dwarf M_⋆ = 0.1 M_⊙, flyby distance d = 120 au; (b) R_d = 150 au, M_⋆ = 0.2 M_⊙, d = 120au; (c) R_d = 100 au, M_⋆ = 0.1, M_⊙, d = 90 au; (d) R_d = 100 au, M_⋆ = 0.2 M_⊙, d = 90 au. The first column illustrates the gas distribution in the entire system ∼2–3 kyr after the flyby. The second column are zoomed-in views of the snapshots in the first column, showing the distribution of captured gas by the M dwarf. The third column shows the morphology of the second-generation disk around the M dwarf after stabilization of the captured material. The fourth column presents gas surface density against distance to the M dwarf in the resulting second-generation disk. The black dashed curves denote the theoretical profile (Appendix A.1) with a logarithmic slope of surface density versus radius being −15/14. The color code indicates orbital eccentricity.