Abstract　 　　  

    With the recent advancement in observations we will soon be able to resolve the central black holes in the Milky Way and in several nearby galaxies to the event-horizon scale. Not only we can detect the shadow casted by the black hole, but we will also be able to image the complex transition region where accretion flow that reaches the event horizon mingles with the ejection of hot ionised plasmoids, and the complex interfacing region where accretion disk meets the launching base of the large-scale jets. The new observations will demand more proper theoretical modelling, in particular, of the treatment in the radiative process and the radiative transport calculations for the central engine of the active galaxies. In this talk I will first discuss about the basic of radiative transfer in relativistic flows subjected to strong gravity. I will show how to obtain the general relativistic radiative transfer formulation in a precise and self-consistent manner based on solid physics foundation. This covariant formulation will give reliable theoretical predictions and provide meaningful interpretations to observations. I will demonstrate how we may apply this formulation in real astrophysical settings. I will present results of the recent calculations carried out my collaboration on general relativistic radiative transfer of emission from accretion inflows and time-dependent outflows near the massive black holes.