Numerical modelling the mass feeding rates on to accretion-modified stars embedded within AGN discs

ABSTRACT Accretion discs surrounding supermassive black holes can potentially form stars within the self-gravitating region. These stars undergo high accretion rates because of the dense environment of the active galactic nuclei (AGNs) accretion disc. The vorticity of the AGN disc may influence the ultimate mass feeding rate towards the star. In our study, we simulate mass feeding rates on to stars at different AGN disc thicknesses through 3D numerical models to explore the relationship between feeding rates and the thermal mass of the star ($q_{\rm th}$), defined as the ratio of the star’s Bondi radius to the AGN disc thickness. Our findings indicate that disc shearing with angular momentum can notably decrease the feeding rate, and we provide an approximate formula that links the feeding rate based on the angular momentum of the surrounding gas and the thermal mass $q_{\rm th}$. Lastly, we examine the potential feedback of the rapidly accreting stars on the AGN disc and their subsequent evolution.