Evolution of the Hubble Sequence in Hierarchical Models for Galaxy   Formation
  We present a model for the broad morphological distinction between the disk and spheroidal components of galaxies. Elaborating on the hierarchical clustering scheme of galaxy formation proposed by Cole et al., we assume that galaxies form stars quiescently in a disk until they are disrupted into a spheroidal configuration by mergers. We calculate formation and merging histories, and the evolution in colour, luminosity and morphology of the galaxy populations in different environments. Roughly $ 50\ %$ of ellipticals in our model have undergone a major merger since $z = 0.5$, yet in spite of this we find that cluster ellipticals have colour-magnitude diagrams with remarkably small scatter. The morphological mix of galaxies that become rich cluster members at high redshift is dominated by spiral galaxies, due to the long timescale for galaxy mergers compared with the timescale for cluster assembly at high redshift. The assembly of low redshift clusters is slower, allowing more galaxy mergers to occur in the progenitor halos. As a result $z=0$ rich clusters become E/S0 dominated and we find a ``Butcher-Oemler'' effect that becomes weaker for poorer groups at high redshift. The field luminosity function of red galaxies shows little evolution out to $z\simeq 1$ and the reddest galaxies at these redshifts are as bright as their local counterparts. The blue luminosity function, on the other hand, evolves rapidly with redshift, increasing its characteristic luminosity and becoming steeper at the faint end. These trends are similar to those recently observed in the Canada-France Redshift Survey. 
C.M. Baugh, S. Cole, C.S. Frenk (Durham University, UK)