Properties of barred spiral disks in hydrodynamical cosmological
  simulations
  We present a quantification of the properties of bars in two N-body+SPH
cosmological simulations of spiral galaxies, named GA and AqC. The initial
conditions were obtained using the zoom-in technique and represent two dark
matter (DM) halos of $2-3\times10^{12}\ {\rm M}_\odot$, available at two
different resolutions. The resulting galaxies are presented in the companion
paper of Murante et al. (2014). We find that the GA galaxy has a bar of length
$8.8$ kpc, present at the two resolution levels even though with a slightly
different strength. Classical bar signatures (e.g. pattern of streaming
motions, high $m=2$ Fourier mode with roughly constant phase) are consistently
found at both resolutions. Though a close encounter with a merging satellite at
$z\sim0.6$ (mass ratio $1:50$) causes a strong, transient spiral pattern and
some heating of the disk, we find that bar instability is due to secular
process, caused by a low Toomre parameter $Q\lesssim1$ due to accumulation of
mass in the disk. The AqC galaxy has a slightly different history: it suffers a
similar tidal disturbance due to a merging satellite at $z\sim0.5$ but with a
mass ratio of $1:32$, that triggers a bar in the high-resolution simulation,
while at low resolution the merging is found to take place at a later time, so
that both secular evolution and merging are plausible triggers for bar
instability.
