  The X-ray light-curves of the GRB afterglows monitored by Swift display one
to four phases of power-law decay. In chronological order they are: the burst
tail, the "hump", the standard decay, and the post jet-break decay.
  The large-angle emission produced during the burst, but arriving at observer
later, is consistent with the GRB tail decay for less than half of bursts. The
forward-shock synchrotron emission from a very narrow jet (half-angle less than
1 deg) is consistent with the decay of 75 percent of GRB tails. The
forward-shock inverse-Compton emission from a narrow jet that does not expand
sideways also accommodates the decay of 80 percent of GRB tails.
  The X-ray light-curve hump can be attributed to an increasing kinetic energy
per solid angle of the forward-shock region visible to the observer. This
increase could be due to the emergence of the emission from an outflow seen
from a location outside its opening. However, the correlations among the hump
timing, flux, and decay index expected in this model are not confirmed by
observations. Thus, the increase in the forward-shock kinetic energy is more
likely caused by some incoming ejecta arriving at the shock during the
afterglow phase.
  The jet interpretation for the burst tails and the energy injection scenario
for the hump lead to a double-jet outflow structure consisting of a narrow GRB
jet which precedes a wider afterglow outflow of lower kinetic energy per solid
angle but higher total energy. (X-ray light-curves are shown for GRB 050416A,
050525A, 050717, 050721, 050724, 050730, 050802, 051109A, 060124, 060206,
060526).
