In this study , with the aid of N-Body simulations based on quasi-cosmological initial conditions , we have followed the formation and evolution of two early-type galaxies of different total mass , from their separation from global expansion of the Universe to their collapse to virialized structures , the formation of stars and subsequent nearly passive evolution .
Using the PD-TSPH N-Body code , we developed the simulations of two model galaxies in quasi-cosmological context .
The cosmological background we have considered is the Standard CDM .
The models are made of Dark and Baryonic Matter in standard cosmological proportions ( 9:1 ) , and have significantly different initial total mass , i.e . 1.62 \times 10 ^ { 12 } M _ { \odot } ( A ) and 0.03 \times 10 ^ { 12 } M _ { \odot } ( B ) .
Particular care has been paid to the star formation process , heating and cooling of gas , and chemical enrichment .
Star formation is completed within the first 3 Gyr in Model A , whereas it lasts longer up to about 4 Gyr in Model B .
The models are followed for a long period of time , i.e .
13 Gyr ( Model A ) and 5 Gyr ( Model B ) : in any case , well beyond the stages of active star formation .
The structural properties of the present-day models are in good agreement with current observations .
The chemical properties , mean metallicity and metallicity gradients also agree with available observational data .
Finally , conspicuous galactic winds are found to occur .
The models conform to the so-called revised monolithic scheme , because mergers of substructures have occurred very early in the galaxy life .
Our results agree with those obtained in other similar recent studies , thus strengthening the idea that the revised monolithic scheme is the right trail to follow in the forest of galaxy formation and evolution .