On the origin of the unique isolated X-Ray pulsar 1E 161348-5055 with 6.7 hr. spin period

A scenario for the formation of an isolated X-ray pulsar 1E161348-5055 with an anomalously long period of 6.7 hours is proposed. It is shown that this pulsar can be a descendant of a massive X-ray binary system, which disintegrated about 2000 years ago after a supernova explosion caused by the core collapse of a massive component. X-ray radiation of this object in the present epoch is generated as a result of accretion of matter onto (about 10 million years old) neutron star from the residual non-Keplerian accretion disk. The pulsar’s nebula RCW 103 is a supernova remnant formed by the explosion of its massive companion in the final evolutionary phase of a massive binary system.