A scenario of the formation of isolated X-ray pulsars is discussed with an application to one of the best studied objects of this class 1E 161348-5055 .
This moderately luminous , 10 ^ { 33 } -10 ^ { 35 } { erg s ^ { -1 } } , pulsar with a relatively soft spectrum , kT \sim 0.6 - 0.8 keV , is associated with an isolated neutron star , which is located near the center of the young ( \sim 2000 yr ) compact supernova remnant RCW 103 and rotates steadily ( | \dot { \nu } | \leq 2.6 \times 10 ^ { -18 } { Hz s ^ { -1 } } ) with the period of 6.7 hr .
We show that in the current epoch the neutron star is in the accretor state .
The parameters of the source emission can be explained in terms of the magnetic-levitation accretion scenario in which the star with the surface magnetic field of 10 ^ { 12 } G accretes material onto its surface from a non-Keplerian magnetic fossil disk at the rate 10 ^ { 14 } { g s ^ { -1 } } .
A neutron star could evolve to this state in a High-Mass X-ray Binary ( HMXB ) , which had disintegrated during the supernova explosion powered by the core-collapse of its massive component .
The life-time of an isolated X-ray pulsar formed this way can be as long as a few thousand years .