**Stefano Borgani**

INFN - Sezione di Trieste, c/o Dipartimento di Astronomia,

via Tiepolo 11, I-34131 Trieste, Italy

In these Lectures I provide general notions about the
formation and evolutions of cosmic structures, like galaxies and
clusters of galaxies, within the standard cosmological scenario,
based on a spatially homogeneous and isotropic expanding
Universe. After briefly reviewing the cinematics and dynamics of
the Friedman-Robertson-Walker model, I introduce the notation
for describing the degree of inhomogeneity which characterizes
the structure of the Universe on scales Mpc, thus much
smaller than the cosmological event horizon ( Mpc).
Afterwards I introduce the basic equations for the evolution of
density perturbations and derive their solution in the linear
case of small perturbations. In this context, I also describe the
evolution of perturbations both in the baryonic and in the
non-baryonic dark matter (DM) component. We explicitely show how
the nature (either cold or hot) of the DM affects the formation
and evolution of cosmic structures. We finally discuss how modern
numerical computational techniques and observations can be joined
together to improve our understanding of the nature of our
Universe and its evolution,

- The standard cosmological model
- Describing the inhomogeneities of the Universe
- The spectrum of primordial fluctuations
- References
- Bibliography
- About this document ...