General relativistic radiative transfer in black hole systems

Abstract

The current work going on to capture the image of the near surroundings of the black hole gets greatly helped when the observational signatures are made in comparison with the dynamical simulations produces by efficient codes. Radiation which are generated from the near surroundings of the black hole passes through the region close to the event horizon of the black hole and arrives at the observer. Our aim is to produce a new open source code which produces accurate representations of the fast moving plasma at relativistic speeds. We have developed our own reverse ray tracing algorithm to produce emission maps of black hole. We have produced these maps for flat accretion disks and also for a tori shaped accretion disk. We have taken a rotationally supported accretion torus for our purpose. We then have produced algorithms to calculate the Doppler shift encountered by each ray coming from the surface of the accreting surface. We then later progressed towards calculating relativistic line profiles for different angles and spin of the black hole for both flat and tori shaped accreting body. Our aim in future is to encorporate polarized radiative transfer ray tracing algorithm in order to understand the morphology of the magnetic field lines in the near surroundins of the black hole.