Quenching, bursting and galaxy shapes: colour transformation as a
  function of morphology
  Different mechanisms for quenching star formation in galaxies are commonly
invoked in the literature, but the relative impact of each one at different
cosmic epochs is still unknown. In particular, the relation between these
processes and morphological transformation remains poorly understood. In this
work, we measure the effectiveness of changes in star formation rates by
analysing a new parameter, the Star Formation Acceleration (SFA), as a function
of galaxy morphology. This methodology is capable of identifying both bursting
and quenching episodes that occurred in the preceding 300 Myrs. We use
morphological classification catalogs based on Deep learning techniques. Our
final sample has $\sim$14,200 spirals and $\sim$2,500 ellipticals. We find that
elliptical galaxies in the transition region have median shorter quenching
timescales ( $\tau$ < 1 Gyr) than spirals ($\tau \geq 1$ Gyr). This result
conforms to the scenario in which major mergers and other violent processes
play a fundamental role in galaxy evolution for most ellipticals, not only
quenching star formation more rapidly but also playing a role in morphological
transformation. We also find that $\sim$two thirds of galaxies bursting in the
green valley in our sample are massive spirals ($M_\star \geq
10^{11.0}M_\odot$) with signs of disturbance. This is in accordance with the
scenario where low mass galaxies are losing their gas in a interaction with a
massive galaxy: while the former is quenching, the last is being refueled and
going through a burst, showing signs of recent interaction.
