Abstract: Adopting the data of high-precision and large-sample \Lambdacold dark matter (\LambdaCDM) cosmological simulations, the effects of baryonicprocesses on the shapes and angular momentum of dark matter (DM) haloshave been investigated.Here, the data of three numerical simulations at three different redshifts were used,i.e., dark matter only (DMO), radiative cooling, star formation, and kinetic supernovaefeedback (CSF), and CSF simulation accompanying with active galactic nucleus (AGN) feedback.The baryonic processes can influence the halo mass function,especially in the presence of AGN feedback.However, the feedback of AGN reduces the formation of massive DM halos.As the Universe evolves, the spatial shapes of DM halos are gradually fromflat to round.The baryonic processes accelerate this process as well as make DM halosmore rounded, while the AGN feedback suppresses this acceleration, and thiseffect of baryonic processes is dependent on both the masses and radii ofDM halos.The smaller masses of DM halos, the more significant effect of baryons will occur.Meanwhile, the baryonic processes contribute to the rounding process forany masses or radii of DM halos, although the AGN feedback will suppress thisfacilitation.In particular, the effect of baryons is particularly pronounced for the DM haloshaving radii at 0.2--0.6 times the virial radius.Besides, the baryonic processes have an effect on the angular momentum ofDM halos, e.g., increases the angular momentum.The spin parameter does not depend on the mass but has a certain correlationwith the radius of the DM halo.