  We present a new model for soft gamma-ray repeaters based on a quark star
born with temperatures above the critical value (T_c) for the onset of the
colour-flavor locked superconductivity. The quark star then quickly cools below
T_c, expelling a fraction of the surface magnetic field via the Meissner
effect. We show that if a small fraction (\leq 10%) of the surface magnetic
field (10^{14} - 10^{15} {\rm G}) is expelled, it quickly decays via magnetic
reconnection and heats up the quark star surface to temperatures > 10^9 {\rm
K}. Created (e^{+},e^{-}) pairs annihilate into gamma rays emitted in a giant
burst (the first burst in our model), with a luminosity of \sim 10^{45} {\rm
ergs} {\rm s}^{-1}. Subsequent bursts result from the restructuring of the
surface magnetic field following the formation and relaxation of a vortex
lattice which confines the internal magnetic field. During this phase, energy
is sporadically released as a consequence of magnetic reconnection events in
the entangled surface magnetic field as it evolves into a smooth, more stable,
configuration. The star eventually enters a quiescent phase in which energy is
continuously supplied by vortex annihilation at the surface. As the star spins
down, the outermost vortex lines will be pushed to the surface where they
annihilate and release their confined magnetic field. We show that the
corresponding luminosity is L_v \sim 10^{36} {\rm ergs} {\rm s}^{-1} for a
typical soft gamma-ray repeater spinning with a period of 8 {\rm s} and a
surface magnetic field not exceeding 10^{15} {\rm G}. Our model can be applied
to any situation where a T>T_{\rm c} quark star is generated. We discuss the
connection between anomalous X-ray pulsars and soft gamma-ray repeaters in the
context of our model.
