The buildup of strongly barred galaxies in the TNG100 simulation
  We analyse the properties of strongly barred disc galaxies using the TNG100
simulation, a cosmological hydrodynamical realisation of the IllustrisTNG
suite. We identify 270 disc galaxies at $z=0$ in the stellar mass range
$M_{*}=10^{10.4-11}M_{\odot}$, of which 40 per cent are barred. Of the detected
bars, more than half are strong. We find that the fraction of barred galaxies
increases with stellar mass, in agreement with observational results. Strongly
barred galaxies exhibit, overall, lower gas-to-stellar mass ratios compared to
unbarred galaxies. The majority of barred galaxies are quenched (sSFR
$\sim10^{-11.7} $yr$^{-1}$), whereas unbarred galaxies continue to be active
(sSFR $\sim10^{-10.3}$yr$^{-1}$) on the main sequence of star-forming galaxies.
We explore the evolution of strongly barred and unbarred galaxies to
investigate their formation and quenching histories. We find that strong bars
form between $0.5< z< 1.5$, with more massive galaxies hosting older bars.
Strong bars form in galaxies with an early-established prominent disc
component, undergoing periods of enhanced star formation and black hole
accretion, possibly assisted by cosmological inflows. Unbarred galaxies, on the
other hand, assemble most of their mass and disc component at late times. The
nuclear region of strongly barred galaxies quenches shortly after bar
formation, while unbarred galaxies remain active across time. Our findings are
indicative of bar quenching, possibly assisted by nuclear feedback processes.
  We conclude that the cosmological environment, together with small scale
feedback processes, determine the chances of a galaxy to form a bar and to
rapidly quench its central region.
