This thesis explores the orbital evolution of an initially thin stellar disc around a supermassive black hole. The results, obtained by both direct numerical N-body modelling and standard perturbation methods, explain the observed configuration of young stars.

This thesis explores the orbital evolution of an initially thin stellar disc around a supermassive black hole. The results, obtained by both direct numerical N-body modelling and standard perturbation methods, explain the observed configuration of young stars.

This thesis explores the orbital evolution of an initially thin stellar disc around a supermassive black hole. The results, obtained by both direct numerical N-body modelling and standard perturbation methods, explain the observed configuration of young stars.