The accretion induced neutron star magnetic field evolution is studied through considering the accretion flow to drag the field lines aside and dilute the polar field strength, and as a result the equatorial field strength increases and is buried inside the crust. The main conclusions of model are as follows: (i) the polar field decays with increasing the accreted mass; (ii) The bottom magnetic field strength of about 10 G can occur when neutron star magnetosphere radius approaches the star radius, which depends on the accretion rate as Ṁ; (iii) The neutron star magnetosphere radius decreases with accretion until it reaches the star radius, and its evolution is little influenced by the initial field and the accretion rate after accreting ∼ 0.01M⊙, which implies that the magnetosphere radii of neutron stars in LMXBs would be homogeneous for Z sources and Atoll sources if they accreted the comparable masses. As an extension, the physics effects of the possible strong magnetic zone in the X-ray neutron stars and recycled pulsars are discussed. Moreover, The the strong magnetic fields in the binary pulsars PSR 1831-00 and PSR 1718-19 after accreting about half solar mass in the binary accretion phase, 8.7× 10 G and 1.28× 10 G, respectively, can be explained through considering the incomplete frozen flow in the polar zone. As a model’s expectation, the existence of the low magnetic field (∼ 3× 10 G) neutron stars or millisecond pulsars is suggested.