Dynamics of Accretion Process Around AGN in Schwarzschild-de Sitter Geometry

Abstract

More recent literature reviews point out that most galaxies, especially early type galaxies with Active Galactic Nuclei (AGNs), contain Massive Black Holes (MBHs) considered to be comparable to the masses of high redshift quasars to the evolution of early galaxies. Some of these sources seem to accrete matter at a very high rate as reported. As a result it is believed that Electromagnetic (EM) spectrum observations are required to provide information on black holes in the centers of active galaxies. On the other hand, Gravitational Wave (GW) observations are considered to provide the complementary information about the capture of particles including compact objects like Black Holes (BHs) that are mostly invisible to EM observations. Thus, the astrophysical study of AGNs in its full relativistic e ect is active and fresh research. For example, the e cient mechanisms to describe the energy - momentum and particles ow of the accretion system that could be exploited to match observations are important and open to research. Motivated by this, we were proposing to study on the dynamics of accretion ow around AGNs. The method we used to derive relevant dynamical parameters from the Lagrangian and Hamiltonian of general relativistic (GR) particle geodesy in the Schwarzschild - de Sitter (SdS) geometry where the classical analogy is adopted by the correspondence principle (CP). The analytically derived equations were used to generate numerical values computationally, where the results discussed and summarized to remark for observational validity.