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In recent years the Sloan Digital Sky Survey has unraveled a new populationof ultra-faint dwarf galaxies (UFDs) in the vicinity of the Milky Way (MW)whose origin remains a puzzle. Using a suite of collisionless N-bodysimulations, we investigate the formation of UFDs in the context of the tidalstirring model for the formation of dwarf spheroidal galaxies in the LocalGroup (LG). Our simulations are designed to reproduce the tidal interactionsbetween MW-sized host galaxies and rotationally supported dwarfs embedded in10^9 M_sun dark matter (DM) halos. We explore a variety of inner density slopes\rho \propto r^{-\alpha} for the dwarf DM halos, ranging from core-like (\alpha= 0.2) to cuspy (\alpha = 1), and different dwarf orbital configurations. Ourexperiments demonstrate that UFDs can be produced via tidal stirring of diskydwarfs on relatively tight orbits, consistent with a redshift of accretion bythe host galaxy of z \sim 1, and with intermediate values for the halo innerdensity slopes (\rho \propto r^{-0.6}). The inferred slopes are in excellentagreement with those resulting from both the modeling of the rotation curves ofdwarf galaxies and recent cosmological simulations of dwarf galaxy formation.Comparing the properties of observed UFDs with those of their simulatedcounterparts, we find remarkable similarities in terms of basic observationalparameters. We conclude that tidal stirring of rotationally supported dwarfsrepresents a viable mechanism for the formation of UFDs in the LG environment.

How to make an ultra-faint dwarf spheroidal galaxy: tidal stirring of disky dwarfs with shallow dark matter density profiles