All Figures

Figure 1: Schematic view of the initial and final stages in the development of the SGR in our model. The QS, born with quickly cools into a CFL star. In the early stages of this transition, a fraction of the surface magnetic field is expelled by the Meissner effect, inducing magnetic reconnection events leading to the main burst. In the late stage, once the vortices form (parallel to the rotation axis), the system evolves into a configuration where most of the magnetic field is confined to the vortex lines. Magnetic reconnection events between the complex surface magnetic field and the external part of the magnetic field coupled to the vortex lines lead to occasional flares (subsequent bursts). In the SGR quiescent phase, magnetic energy is released as vortex lines are being continuously pushed to the surface and annihilate there. In the more general case where the magnetic field is not aligned with the rotation axis, we expect an even more complex behaviour/evolution of the field leading to more reconnection events.

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In the text

	Figure 2: The light curve expected in our model. The four curves (from top to bottom) correspond to , 0.2, 0.1, and 0.05.
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In the text

	Figure 3: Upper panel: the light curve for . Lower panel: the corresponding time evolution of the surface temperature.
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In the text

	Figure 4: The X-ray luminosity versus period for the four SGRs for which these values have been measured (from Kaplan 2000, and references therein). The solid lines are predictions given by Eq. (24) for stars with magnetic fields of (upper curve) and , for and . The dashed lines are predictions given by Eq. (25) for stars with magnetic fields of (upper curve) and  , for .
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In the text