Star formation at the Galactic Centre: coevolution of multiple young
  stellar discs
  Studies of the Galactic Centre suggest that in-situ star formation may have
given rise to the observed stellar population near the central supermassive
black hole (SMBH). Direct evidence for a recent starburst is provided by the
currently observed young stellar disc (2-7 Myr) in the central 0.5 pc of the
Galaxy. This result suggests that star formation in galactic nuclei may occur
close to the SMBH and produce initially flattened stellar discs. Here we
explore the possible build-up and evolution of nuclear stellar clusters near
SMBHs through in-situ star formation producing stellar discs similar to those
observed in the Galactic Centre and other nuclei. We make use of N-body
simulations to model the evolution of multiple young stellar discs and explore
the potential observable signatures imprinted by such processes. Each of the
five simulated discs is evolved for 100 Myr before the next one is introduced
in the system. We find that populations born at different epochs show different
morphologies and kinematics. Older and presumably more metal poor populations
are more relaxed and extended, while younger populations show a larger amount
of rotation and flattening. We conclude that star formation in central discs
can reproduce the observed properties of multiple stellar populations in
galactic nuclei differing in age, metallicity and kinematic properties.
