  The existence of dwarf spheroidal galaxies with high internal velocity
dispersions orbiting in the Milky Way raises questions about their dark matter
content and lifetime. In this paper, we present an alternative solution to the
dark matter dominated satellites proposed by Ibata & Lewis (1998) for the
Sagittarius dwarf galaxy. We performed simulations of two kinds of N-body
satellites: the first models (f-models) could correspond to satellites with
high dark matter content and they represent initially isolated models. The
second models (s-models) have either low or negligible dark matter content and
they are constructed in a tidal field. In spite of being on the same orbits,
the s-models are able to produce a better agreement with some observational
constraints concerning Sagittarius. From our simulations, we can also infer
that Sagittarius is in the process of being disrupted.
