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The formation of dwarf spheroidal galaxies in the Local Group from diskyprogenitors via tidal interaction with a bigger host is one of the mostpromising scenarios of their origin. Using N-body simulations we study theprocess by following the evolution of a disky dwarf orbiting a Milky Way-likehost. We focus on the effect of the orientation of the dwarf galaxy disk'sangular momentum with respect to the orbital one. We find a strong dependenceof the efficiency of the transformation from a disk to a spheroid on the diskorientation. The effect is strongest for the exactly prograde and weakest forthe exactly retrograde orbit. In the prograde case the stellar component formsa strong bar and remains prolate until the end of the evolution, while itsrotation is very quickly replaced by random motions of the stars. In theretrograde case the dwarf remains oblate, does not form a bar and losesrotation very slowly. Our results suggest that resonant effects are the mostimportant mechanism underlying the evolution while tidal shocking plays only aminor role.

Tidal evolution of disky dwarf galaxies: prograde versus retrograde orbits