  We describe a model within the ``Quark-nova'' scenario to interpret the
recent observations of early X-ray afterglows of long Gamma-Ray Bursts (GRB)
with the Swift satellite. This is a three-stage model within the context of a
core-collapse supernova. STAGE 1 is an accreting (proto-) neutron star leading
to a possible delay between the core collapse and the GRB. STAGE 2 is accretion
onto a quark-star, launching an ultrarelativistic jet generating the prompt
GRB. This jet also creates the afterglow as the jet interacts with the
surrounding medium creating an external shock. Slower shells ejected from the
quark star (during accretion), can re-energize the external shock leading to a
flatter segment in the X-ray afterglow. STAGE 3, which occurs only if the
quark-star collapses to form a black-hole, consists of an accreting black-hole.
The jet launched in this accretion process interacts with the preceding quark
star jet, and could generate the flaring activity frequently seen in early
X-ray afterglows. Alternatively, a STAGE 2b can occur in our model if the quark
star does not collapse to a black hole. The quark star in this case can then
spin down due to magnetic braking, and the spin down energy may lead to
flattening in the X-ray afterglow as well. This model seems to account for both
the energies and the timescales of GRBs, in addition to the newly discovered
early X-ray afterglow features.
