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Disk Accretion onto Magnetized Neutron Stars: The Inner Disk Radius and Fastness Parameter | | X.-D. Li
; Z.-R. Wang
; | | Date: |
8 Dec 1998 | | Subject: | astro-ph | | Affiliation: | Department of Astronomy, Nanjing University | | Abstract: | It is well known that the accretion disk around a magnetized compact star can penetrate inside the magnetospheric boundary, so the magnetospheric radius $
o$ does not represent the true inner edge $
in$ of the disk; but controversies exist in the literature concerning the relation between $
o$ and $
in$. In the model of Ghosh & Lamb, the width of the boundary layer is given by $delta=
o-
inll
o$, or $
insimeq
o$, while Li & Wickramasinghe recently argued that $
in$ could be significantly smaller than $
o$ in the case of a slow rotator. Here we show that if the star is able to absorb the angular momentum of disk plasma at $
o$, appropriate for binary X-ray pulsars, the inner disk radius can be constrained by $0.8lsim
in/
olsim 1$, and the star reaches spin equilibrium with a relatively large value of the fastness parameter ($sim 0.7-0.95$). For accreting neutron stars in low-mass X-ray binaries (LMXBs), $
o$ is generally close to the stellar radius $
s$ so that the toroidal field cannot transfer the spin-up torque efficiently to the star. In this case the critical fastness parameter becomes smaller, but $
in$ is still near $
o$. | | Source: | arXiv, astro-ph/9901083 | | Services: | Forum | Review | PDF | Favorites | |
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