Planned Project

Our next plan is to formulate the most general model for accretion powered relativistic MHD jet formation. We would like to start by writing the relativistic energy momentum tensor for compressible fluid with shear and bulk viscosity, with mutual energy exchange in between internal fluid elements and radiative energy exchange in between the fluid and the surrounding. Practically, such an energy momentum tensor should be the combination of the individual energy momentum tensors representing the matter field and the Maxwell stress-energy tensor associated with the $\overline{\bf B}$ field. We plan to use the Boyar Lindquist co-ordinate with an azimuthally Lorentz boosted orthonormal tetrad basis co-rotating with the accreting fluid, and consider gravo-magneto-viscous non-alignment between the specific flow angular momentum of accreting matter and the black hole spin angular momentum (the Kerr parameter $a$) to include the Bardeen Paterson Effect as well. Solution of the above equation will lead to the equations governing the energy, mass, and the linear and angular momentum of the accretion flow.

The next step would be to construct the representative equations for general relativistic MHD shocks. Such set of equations, which fully governs the flow, will be highly non-linearly coupled and non-exactly solvable. At this stage, numerical techniques will be employed to simultaneously solve the set of equations governing the accretion flow along with the relativistic MHD shock conditions. Initially our work will concentrate on axisymmetric stationary solutions to investigate the formation of standing shocks and to study how such shock solutions produces outflow. Subsequently, we will introduce time dependence in our solution scheme to study how such shock oscillates (depending on the relative magnitude of the post-shock cooling and advection time scale) to produce the quasi periodic oscillation (QPO) in galactic sources harbouring stellar mass black holes.