  Inspired by recent work on feedback in disk galaxies (Efstathiou 2000, Silk
2003) and on the angular momentum distribution in simulated gas halos (Sharma
and Steinmetz 2005), a fully dynamic model of disk galaxy formation and
evolution has been developed. This is used to demonstrate how observed galactic
systems could have formed from halos similar to those found in simulations and
applies physically motivated models of star formation and feedback to explore
whether the true nature of these processes would be manifest from local and
cosmological observables. This is made possible by computational integration
with the galaxy formation model developed originally by the group at Durham
University (Cole et al. 2000).
