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(abridged) The Milky Way (MW) and Andromeda (M31) galaxies possess rotatingplanes of satellites. Their formation has not been explained satisfactorilyyet. It was suggested that the MW and M31 satellites are ancient tidal dwarfgalaxies, which could explain their configuration. This suggestion gainedsupport by an analytic backward calculation of the relative MW-M31 orbit in theMOND modified dynamics paradigm by Zhao et al. (2013) implying their closeflyby 7-11 Gyr ago. Here we explore the Local Group history in MOND in moredetail using a simplified first-ever self-consistent simulation. We note thefeatures induced by the encounter in the simulation and identify their possiblereal counterparts. The simulation was set to approximately reproduce theobserved MW and M31 masses, effective radii, separation, relative velocity anddisk inclinations. We used the publicly available adaptive-mesh-refinement codePhantom of RAMSES. In the simulation, matter was transferred from the MW to M31along a tidal tail. The encounter induced formation of several structuresresembling the peculiarities of the Local Group. Most notably: 1) A rotatingplanar structure formed around M31 from the transferred material. It had a sizesimilar to the observed satellite plane and was oriented edge-on to thesimulated MW, just as the real one. 2) The same structure also resembled thetidal features observed around M31 by its size and morphology. 3) A warp in theMW developed with an amplitude and orientation similar to that observed. 4) Acloud of particles formed around the simulated MW, with the extent of theactual MW satellite system. The encounter did not end by merging in a Hubbletime. The simulation thus demonstrated that MOND can possibly explain manypeculiarities of the Local Group and, moreover, that non-merging galaxyencounters in MOND can produce tidal features in galaxies.

MOND simulation suggests the origin of some peculiarities in the Local Group