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The X-ray source 1E 161348-5055 in the supernova remnant RCW 103 recentlyexhibited X-ray activity typical of magnetars, i.e. neutron stars with magneticfields > 10^14-10^15 G. However, 1E 161348-5055 has an observed period of 6.67hr, in contrast to magnetars which have a spin period of seconds. Here wedescribe a simple model which can explain the spin evolution of 1E 161348-5055,as well as other magnetars, from an initial period of milliseconds that wouldbe required for dynamo generation of magnetar-strength magnetic fields. Wepropose that the key difference between 1E 161348-5055 and other magnetars isthe persistence of a remnant disk of small total mass. This disk caused 1E161348-5055 to undergo ejector and propeller phases in its life, during whichstrong torques caused a rapid increase of its spin period. By matching itsobserved spin period and ~1-3 kyr age, we find that 1E 161348-5055 has the(slightly) highest magnetic field of all known magnetars, with B~5x10^15 G, andthat its disk had a mass of ~10^24 g, comparable to that of the asteroid Ceres.

Ejector and propeller spin-down: How might a superluminous supernova millisecond magnetar become the 6.67 hr pulsar in RCW103