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We provide a set of numerical N-body simulations for studying the formationof the outer Milky Ways's stellar halo through accretion events. Aftersimulating minor mergers of prograde and retrograde orbiting satellite halowith a Dark Matter main halo, we analyze the signal left by satellite stars inthe rotation velocity distribution. The aim is to explore the orbitalconditions where a retrograde signal in the outer part of the halo can beobtained, in order to give a possible explanation of the observed rotationalproperties of the Milky Way stellar halo. Our results show that, for satellitesmore massive than $\sim 1/40$ of the main halo, the dynamical friction has afundamental role in assembling the final velocity distributions resulting fromdifferent orbits and that retrograde satellites moving on low inclinationorbits deposit more stars in the outer halo regions end therefore can producethe counter-rotating behavior observed in the outer Milky Way halo.

Assembly of the outer Galactic stellar halo in the hierarchical model