We consider the early cooling evolution of strongly magnetized strange stars in a CFL phase with high gap \Delta \stackrel { \scriptstyle > } { \phantom { } { } _ { \sim } } 100 MeV .
We demonstrate how this model may explain main features of the gamma-ray burst phenomena and also yield a strong star kick .
The mechanism is based on beaming of neutrino emission along the magnetic vortex lines .
We show that for sufficiently high initial temperatures T _ { 0 } \sim 30 to 60 ~ { } MeV and surface magnetic fields B _ { s } \sim 10 ^ { 15 } to 10 ^ { 17 } ~ { } G , the energy release within the narrow beam is up to 10 ^ { 52 } erg with a magnetic field dependent time scale between 10 ^ { -2 } s ( for a smaller magnetic field ) to 10 s. The above mechanism together with the parity violation of the neutrino-producing weak interaction processes in a magnetic field allow for the strange star kick .
The higher the magnetic field the larger is the stars kick velocity .
These velocities may cover the same range as observed pulsar kick velocities .