rather special making the merger highly improbable. In this paper we aim to investigate how much these conditions may be relaxed and still reproduce the prolate rotation in the final product of the merger. We study the effect of different initial inclination angles of the dwarf disks and the effect of non-radial orbits of the dwarfs. In section 2 we present the simulations used in this study. The orbital evolution of the dwarfs is described in section 3 while their shapes and kinematics in section 4. Section 5 is devoted to a more detailed study of the orbital structure of the remnants. In section 6 we compare the predictions of the scenario based on mergers with an alternative way to form dSph galaxies that relies on their interaction with a bigger host. In section 7 we compare our predictions to the real data for And II and remark on the possible future, more complete model that will describe all the available data. The summary and concluding remarks follow in section 8.

Simulations
===========

We performed five collisionless simulations of mergers between two identical dwarf galaxies. The simulations differed in the initial inclinations of the disks in the dwarfs and their 