The origin of magnetized neutron stars in bineries and the 1.55 ms pulsar is examined in terms of the magnetic field decay model for radio pulsars with a decay time scale of order 5 x 10 to the 6th yr over 7-10 e-foldings. Observational data of pulsing X-ray sources, nonpulsing X-ray sources, and binary radio pulsars are analyzed. Evolutionary scenarios for Her X-1, MXB 1730-335, 4U 1626-67, GX 1 + 4, 1E 2259 + 59, and long-period binary pulsars are described. The data reveal that: magnetic field strengths for accretion-powered X-ray pulsars in massive binaries and rotation-powered radio pulsars in short-period binaries support the formation of these neutron stars by core collapse following the Fe photodisintegration phase of a He-core remnant that resulted from mass transfer; however, the magnetic field strengths for neutron stars low-mass X-ray binaries and in wide radio pulsar binaries are explained if the magnetized neutron stars were formed less than 10 to the 8th years ago by accretion-induced collapse of a massive white dwarf. It is noted that with these two formation models all observations of the magnetic fields of neutron star in binaries are consistent with one single-field decay time scale consistent with one single-field decay time scale down to a surface field strength of less than or equal to 3 x 10 to the 9th G.
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Taam et al. (1986) studied this question.