Astronomy and Astrophysics – Astrophysics
Scientific paper
2004-10-10
Mon.Not.Roy.Astron.Soc. 366 (2006) 137-143
Astronomy and Astrophysics
Astrophysics
8 pages, 4 figs, accepted by MNRAS, 2005
Scientific paper
10.1111/j.1365-2966.2005.09802.x
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 $10^8$ G can occur when neutron star magnetosphere radius approaches the star radius, which depends on the accretion rate as $\mdot^{1/2}$; (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 $\sim 0.01 \ms$, 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 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, $8.7\times10^{10}$ G and $1.28\times10^{12}$ 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 ($\sim 3\times 10^{7}$ G) neutron stars or millisecond pulsars is suggested.
Kojima Yasufumi
Zhang Cheng-Min
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