Abstract
The persistent X-ray pulsar OAO 1657-415 is associated with a wind-fed High Mass X-ray Binary system and shows a peculiar spin evolution. On a timescale of more than 30 years it is observed to experience a regular spin-up which is superposed on episodic and chaotic variations of the period at a very high rate. We explore a possibility to explain the spin evolution of the pulsar in terms of Magnetic Levitation Accretion scenario in which the neutron star captures material from a magnetized stellar wind of its massive companion and accretes matter from a non-Keplerian magnetized disk (Magnetic Levitating disk or ML-disk). We show this scenario to be applicable if the magnetic field in the wind at a distance of binary separation lies in the interval 20 – 70 mG.
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