Formation of relativistic outflows in advection-dominated accretion disks with shocks

Relativistic jets (outflows) are ubiquitous in the observed universe, especially in astrophysical objects, ranging from active galactic nuclei (AGNs) to young stellar objects. In particular, radio-loud AGNs have been receiving much attention due to their powerful outflows. As a consequence, the question of the origin of the high energy particles has been intensively studied. Furthermore, it has been widely believed that accreting black holes are the central engine of AGNs and the accretion is thought to be the origin of the X-ray and gamma-ray emissions and of the jets emerging from AGNs. Much progress has been made in analyzing the disk/jet connection and there is a great consensus among researchers that there are accretion disks in AGNs and the jets/outflows are powered by the accretion disks. Even though some insight has been gained in understanding the origin and the exact acceleration mechanisms powering the outflows/jets, a single, global, self-consistent model for the disk/jet structure is still lacking.; The goals of this thesis are to develop (1) the dynamical flow conservation equations for the gas in inviscid disks, including shocks to describe the relativistic particles acceleration process, (2) a self-consistent transport equation describing both the particles acceleration mechanism that powers the outflows and the escape of matter and energy, and (3) the algorithms that numerically solve the dynamical flow conservation equations and the transport equation self-consistently. The results obtained from these studies will provide us some insight concerning (1) the inner flow structure of the inviscid disks, (2) the connection between the disk and its outflows, and (3) the acceleration process occurring in the disk which powers the outflows.