According to the standard cosmological model, structure formation occurs in a bottom up fashion, where small galaxies are formed first while bigger systems grow by continuous aggregation of smaller ones.
Both observations and theoretical predictions of the galaxy mass function agree on the fact that dwarfs are the most numerous galaxies in the Universe.

Dwarf galaxies are extremely Dark Matter (DM) dominated objects,  containing approximately 2 to 3 orders of magnitude more DM mass than stars. This makes them extremely good laboratories to test the nature of DM.

Moreover, the low mass of dwarf galaxies is not enough to create extremely deep gravitational wells. These shallow gravitational potentials are relatively easily perturbed either by gas outflows triggered by stellar SuperNovae (SN) or by tidal interactions with their environment. Due to the co-evolution of the DM and baryonic content of galaxies, a detailed analysis of the baryonic properties of dwarfs can help to better constrain the properties of the DM and vice-versa.

In this thesis, I aim to better understand how the different parameters involved in the evolution of dwarf galaxies define their properties in the local Universe.
In particular, I have focused the analysis on giving detailed predictions of the chemo-dynamical properties of simulated Ultra Diffuse Galaxies from the NIHAO simulations suite; I have proven the merger origin of stellar prolate rotations in classical dwarfs using GEAR simulation and, finally, I have revised the anti-correlation that appears to happen in the Milky Way satellites between the  central DM density and the pericentric distance, with data collected from the literature.