  Magnetar giant flares show oscillatory modulations in the tails of their
light curves, which can only be explained via some form of beaming. The
fireball model for magnetar bursts has been used successfully to fit the
phase-averaged light curves of the tails of giant flares, but so far no
attempts have been made to fit the pulsations. We present a relatively simple
numerical model to simulate beaming of magnetar flare emission. In our
simulations, radiation escapes from the base of a fireball trapped in a dipolar
magnetic field, and is scattered through the optically thick magnetosphere of
the magnetar until it escapes. Beaming is provided by the presence of a
relativistic outflow, as well as by the geometry of the system. We find that a
simple picture for the relativistic outflow is enough to create the pulse
fraction and sharp peaks observed in pulse profiles of magnetar flares, while
without a relativistic outflow the beaming is insufficient to explain giant
flare rotational modulations.
