Ejector and propeller spin-down: how might a superluminous supernova millisecond magnetar become the 6.67 h pulsar in RCW 103

Abstract

Abstract The X-ray source 1E 161348−5055 in the supernova remnant RCW 103 recently exhibited X-ray activity typical of magnetars, i.e. neutron stars with magnetic fields ≳ 1014–1015 G. However, 1E 161348−5055 has an observed period of 6.67 h, in contrast to magnetars which have a spin period of seconds. Here we describe 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 would be required for dynamo generation of magnetar-strength magnetic fields. We propose that the key difference between 1E 161348−5055 and other magnetars is the persistence of a remnant disc of small total mass. This disc caused 1E 161348−5055 to undergo ejector and propeller phases in its life, during which strong torques caused a rapid increase of its spin period. By matching its observed 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 ∼ 5 × 1015 G, and that its disc had a mass of ∼1024 g, comparable to that of the asteroid Ceres.