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

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 > 10^14-10^15 G. However, 1E 161348-5055 has an observed period of 6.67 hr, 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 disk of small total mass. This disk 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~5x10^15 G, and that its disk had a mass of ~10^24 g, comparable to that of the asteroid Ceres.

5 pages, 3 figures; accepted for publication in MNRAS Letters; v2, minor edits and references added

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Cited by in corpus (5)

• Central Compact Objects in Supernova Remnants
• Comparing Neutron Star Kicks to Supernova Remnant Asymmetries
• Targeted search for young radio pulsars in the SMC: Discovery of two new pulsars
• On the fallback disk around the slowest isolated pulsar, 1E 161348$-$5055
• Long X-ray flares from the central source in RCW 103