Poster Title: Dynamical evolution of stars formed in accretion disks around super-massive black holes
Abstract: The standard accretion theory predicts that the outer parts (R $\ge 1000 R_{S}$) of QSO disks are self-gravitating and should form stars. Recent observations of our own Galactic Centre showed the presence of many young hot stars confined to two well defined rings of truly nuclear scale ( $<$ 0.1 pc). This lends support to theories of star formation in accretion disks, but also begs for an investigation of the star-disk system especially if the disk orientation changes with time. Using analytical estimates and numerical integration, we try to answer some of the basic questions here, such as whether the stars will be confined to the disk plane, whether the disk friction or the N-body effects will dominate the velocity dispersion and the formation of stellar groups, and what is the feedback of the stars on the disk temporal evolution.
Link to poster: N/A