Physics of Supermassive Disks: Formation and Collapse

Abstract

Supermassive disks are thought to be precursors of supermassive black holes that are believed to power quasars and exist at centers of galaxies. Formation scenarios of such disks are reviewed and it is argued that gas dynamical schemes are favourable compared to stellar dynamical schemes which could however be important feeding mechanisms for the growth of the black hole. A new self-similar model of a collapse of a self-gravitating disk due to radiation induced stresses applicable to two different situations of radiative viscosity and Compton drag is presented. The collapse timescale purely due to radiative viscosity is found to be a fraction of Hubble time, $τ_γ\sim{σ_T c/ (m_p G)} ({L_{edd}/ L}) \simeq 6 \times 10^9$yrs is slow and probably magnetic fields play an important role before general relativistic effects take over. A model of self-gravitating disk collapsing due to Compton drag by the Cosmic Microwave Background is also presented which is found to be effective at redshifts $1400>z\gsim 300$. It is proposed that the small $\lsim 10^5 \Msun$ objects that form by this mechanism by $z \sim 20$ can merge and coalesce by dynamical friction to form the high redshift quasars seen. Supermassive stars which are systems (and could be end products of a supermassive disk phase) en route to the final collapse are also briefly reviewed.