Exploring Relativistic Accretion Flow Around Black Holes and Wormholes

Abstract

The origin of high energy radiation from quasars, AGNs, and black hole (BH) X-ray binaries has drawn the attention to the scientific community. Accretion onto compact objects has emerged as a fundamental mechanism in explaining the observed luminosity from those sources. Since the emitted radiation carries imprints of the spacetime geometry near the compact object, the accretion dynamics provide crucial insights into both the nature of the central object and the accreting matter. There are various accretion models, such as Bondi flow, standard thin disk, two-temperature SLE disk, slim disks, ADAFs, but none of them can fully explain both the spectral and timing properties of compact objects. The TCAF model incorporates shock transition due to centrifugal barrier, which forms a post-shock corona (PSC) of hot and dense electrons. This corona can explain the observed high energy radiations via inverse Comptonization of the soft disk photons. Accurate modeling of such flow requires effective potential around compact objects to incorporate the strong gravity. Recently, DDMC potential has been developed to study relativistic hydrodynamics across the entire spin parameter range in stationary, axisymmetric spacetime.