An Overview of the Effect of Self-Gravity on the Structure of Accretion Discs

Abstract

In astrophysical systems like X-ray binaries (XRBs), active galactic nuclei (AGN), and young stellar objects (YSOs), we often observe a very fundamental structure called accretion discs(ADs). Conventional AD theory usually supposes that the gravitational field is controlled by a central compact object. This assumption breaks down when the mass of the disc becomes considerable in contrast to that of the massive central object. In these cases, the AD's self-gravity (SG) can drastically change its structure, dynamics, and evolution. This review investigates how SG influences the radial and vertical structure of ADs and how it modifies the mechanisms that transport angular momentum (AM). Along with these, this review also tries to explore how gravitational instabilities (GIs) evolve and how they affect disc fragmentation and astrophysical phenomena like stellar and planetary formation, AGN dynamics, and gamma-ray bursts (GRBs).