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Disk Accretion onto Magnetized Neutron Stars: the Inner Disk Radius and Fastness Parameter
| Content Provider | Semantic Scholar |
|---|---|
| Author | Wang, Ziqiang |
| Abstract | It is well known that the accretion disk around a magnetized compact star can penetrate inside the magnetospheric boundary, so the magnetospheric radius R 0 does not represent the true inner edge R in of the disk; but controversies exist in the literature concerning the relation between R 0 and R in. In the model of Ghosh & Lamb, the width of the boundary layer is given by δ = R 0 − R in ≪ R 0 , or R in ≃ R 0 , while Li & Wickramasinghe recently argued that R in could be significantly smaller than R 0 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 R 0 , appropriate for binary X-ray pulsars, the inner disk radius can be constrained by 0.8 < ∼ R in /R 0 < ∼ 1, and the star reaches spin equilibrium with a relatively large value of the fastness parameter (∼ 0.7 − 0.95). For accreting neutron stars in low-mass X-ray binaries (LMXBs), R 0 is generally close to the stellar radius R * 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 R in is still near R 0 . |
| File Format | PDF HTM / HTML |
| Alternate Webpage(s) | http://arxiv.org/pdf/astro-ph/9901083v1.pdf |
| Language | English |
| Access Restriction | Open |
| Subject Keyword | AngularJS Bone structure of radius Diagnostic radiologic examination GUCY2C protein, human Kind of quantity - Equilibrium Lithium Natural Science Disciplines Neutrons Plasma Active Population Parameter Small Stars, Celestial Stellar (payment network) Toroidal graph width |
| Content Type | Text |
| Resource Type | Article |
