  We investigate the origins of galaxy morphology (defined by bulge-to-total
K-band luminosity) in the LambdaCDM cosmology using two galaxy formation models
,based on the Millennium simulation, by Bower et al. (the Durham model) and De
Lucia & Blaizot (the MPA model). There are many similarities, but also
fundamental disagreements in the predictions of the two models for galaxy
morphology. For example, taking into account uncertainties in the available
observational data, both produce a realistic morphological mix today, but its
evolution is very different. A main cause of this and other differences is the
treatment of disk instabilities which play a more prominent role in the Durham
model. Our analysis confirms previous theoretical predictions that elliptical
galaxies form most of their stars before the bulk of the galaxy is assembled.
Spirals tend to have later `assembly' times as a consequence of in-situ star
formation. With the exception of the brightest ellipticals (stellar mass >
2.5e11 M_sun/h), we find that major mergers are not the primary mechanism by
which most spheroids (ellipticals and spiral bulges) assemble their mass. In
fact, the majority of ellipticals (and the overwhelming majority of spirals)
never experience a major merger (above the resolution limit of our simulation.)
Most ellipticals and spiral bulges acquire their stellar mass through minor
mergers or disk instabilities. These conclusions are common to both models. The
rotation properties of spheroids may help to constrain the importance of disk
instabilities in these models.

Astrophysics