  We present a simple model for low-mass planet formation and subsequent
evolution within "transition" discs. We demonstrate quantitatively that the
predicted and observed structure of such discs are prime birthsites of planets.
Planet formation is likely to proceed through pebble accretion, should a
planetary embryo ($M\gtrsim 10^{-4}\,$M$_\oplus$) form. Efficient pebble
accretion is likely to be unavoidable in transition disc dust traps, as the
size of the dust particles required for pebble accretion are those which are
most efficiently trapped in the transition disc dust trap. Rapid pebble
accretion within the dust trap gives rise, not only to low-mass planets, but to
a large accretion luminosity. This accretion luminosity is sufficient to heat
the disc outside the gravitational influence of the planet and makes the disc
locally baroclinic, and a source of vorticity. Using numerical simulations we
demonstrate that this source of vorticity can lead to the growth of a single
large scale vortex in $\sim 100$ orbits, which is capable of trapping
particles. Finally, we suggest an evolutionary cycle: planet formation proceeds
through pebble accretion, followed by vortex formation and particle trapping in
the vortex quenching the planetary accretion and thus removing the vorticity
source. After the vortex is destroyed the process can begin anew. This means
transition discs should present with large scale vortices for a significant
fraction of their lifetimes and remnant planets at large ~10AU separation
should be a common outcome of this cycle.
