In this PhD thesis, which was nominated for publication in this
series by the Astronomical Institute at Charles University, Prague,
the author investigates the orbital evolution of an initially thin
stellar disc around a supermassive black hole, considering various
perturbative sources of gravity. His findings, obtained by both
direct numerical N-body modelling and using standard perturbation
methods, offer a viable theoretical explanation for the observed
configuration of young stars in the Galactic Centre. This marks a
significant contribution to a topic of great interest in
contemporary astrophysics. The author also shows in his thesis that
a secular instability (m = 1 mode) may occur in the embedding
spherical cluster of old stars. This increases the richness of
possible evolution scenarios of the embedding cluster and may lead
to effective feeding of supermassive black holes through tidal
disruption of stars on extremely eccentric orbits.
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