The X-ray and radio flares observed in X-ray binaries and active galactic
nuclei (AGN) are attributed to energetic electrons in the plasma ejecta from
the accretion flows near the black hole in these systems. It is argued that
magnetic reconnection could occur in the coronae above the accretion disk
around the black hole, and that this drives plasmoid outflows resembling the
solar coronal mass ejection (CME) phenomenon. The X-ray and radio flares are
emission from energetic electrons produced in the process. As the emission
region is located near the black hole event horizon, the flare emission would
be subject to special- and general-relativistic effects. We present
calculations of the flaring emission from plasmoids orbiting around a black
hole and plasmoid ejecta launched from the inner accretion disk when
general-relativistic effects are crucial in determining the observed
time-dependent properties of the emission. We consider fully
general-relativistic radiative transfer calculations of the emission from
evolving ejecta from black hole systems, with proper accounting for
differential arrival times of photons emitted from the plasmoids, and determine
the emission lightcurves of plasmoids when they are in orbit and when they
break free from their magnetic confinement. The implications for interpreting
time-dependent spectroscopic observations of flaring emission from accreting
black holes are discussed.Comment: 18 pages, 15 figures; Accepted for publication in MNRA