  In a previous paper (Ouyed et al. 2004) we presented a new model for soft
gamma-ray repeaters (SGR), based on the onset of colour superconductivity in
quark stars. In this model, the bursts result from the reorganization of the
exterior magnetic field following the formation of vortices that confine the
internal magnetic field (the \mz effect). Here we extend the model by
presenting full 3-dimensional simulations of the evolution of the inclined
exterior magnetic field immediately following vortex formation. The simulations
capture the violent reconnection events in the entangled surface magnetic field
as it evolves into a smooth, more stable, configuration which consists of a
dipole field aligned with the star's rotation axis. The total magnetic energy
dissipated in this process is found to be of the order of $10^{44}
\mathrm{erg}$ and, if it is emitted as synchrotron radiation, peaks typically
at $280 \mathrm{keV}$. The intensity decays temporally in a way resembling SGRs
and AXPs (anomalous X-ray pulsars), with a tail lasting from a few to a few
hundred times the rotation period of the star, depending on the initial
inclination between the rotation and dipole axis. One of the obvious
consequences of our model's final state (aligned rotator) is the suppression of
radio-emission in SGRs and AXPs following their bursting era. We suggest that
magnetar-like magnetic field strength alone cannot be responsible for the
properties of SGRs and AXPs, while a quark star entering the ``Meissner phase''
is compatible with the observational facts. We compare our model to
observations and highlight our predictions.
