The star formation rate and stellar content contributions of
  morphological components in the EAGLE simulations
  The Hubble sequence provides a useful classification of galaxy morphology at
low redshift. However, morphologies are not static, but rather evolve as the
growth of structure proceeds through mergers, accretion and secular processes.
We investigate how kinematically defined disc and spheroidal structures form
and evolve in the EAGLE hydrodynamic simulation of galaxy formation. At high
redshift most galaxies of all masses are asymmetric. By redshift $z\simeq 1.5$
the Hubble sequence is established and after this time most of the stellar mass
is in spheroids whose contribution to the stellar mass budget continues to rise
to the present day. The stellar mass fraction in discs peaks at $z\simeq 0.5$
but overall remains subdominant at all times although discs contribute most of
the stellar mass in systems of mass $M^*\sim 10^{10.5}{\rm M_\odot}$ at $z \leq
1.5$. Star formation occurs predominantly in disc structures throughout most of
cosmic time but morphological transformations rearrange stars, thus
establishing the low-redshift morphological mix. Morphological transformations
are common and we quantify the rates at which they occur. The rate of growth of
spheroids decreases at $z < 2$ while the rate of decay of discs remains roughly
constant at $z < 1$. Finally, we find that the prograde component of galaxies
becomes increasingly dynamically cold with time.
