  The point X-ray source 1E 161348-5055 is observed to display pulsations with
the period 6.67 hr and |\dot{P}| \leq 1.6 x 10^{-9} s/s. It is associated with
the supernova remnant RCW\,103 and is widely believed to be a ~2000 yr old
neutron star. Observations give no evidence for the star to be a member of a
binary system. Nevertheless, it resembles an accretion-powered pulsar with the
magnetospheric radius ~3000 km and the mass-accretion rate ~ 10^{14} g/s. This
situation could be described in terms of accretion from a (residual) fossil
disk established from the material falling back towards the star after its
birth. However, current fall-back accretion scenarios encounter major
difficulties explaining an extremely long spin period of the young neutron
star. We show that the problems can be avoided if the accreting material is
magnetized. The star in this case is surrounded by a fossil magnetic slab in
which the material is confined by the magnetic field of the accretion flow
itself. We find that the surface magnetic field of the neutron star within this
scenario is ~10^{12} G and that a presence of > 10^{-7} M_\sun magnetic slab
would be sufficient to explain the origin and current state of the pulsar.
