Abstract
Matter spiralling through an accretion disk towards a magnetized neutron star has three ways to go: it can (i) be centrifugally re-expelled, (ii) join a ‘blade’ to spiral all the way in, or (iii) reach a ‘downward’ leading magnetic field line by evaporation. Predominance of channel (ii) over channel (iii) may give rise to non-pulsing sources. Channel (i) may be responsible for the QPO phenomenon.
Whenever the neutron star’s spin is not exactly aligned with that of the binary orbit, magnetic pressures will tilt the inner disk. The mode of decomposition of the disk by the corotating magnetosphere, at its inner edge, should depend not only on the accretion rate and illumination but also on the spin inclination and obliquity of the magnetic dipole moment. An oscillating tilt angle may cause the superorbital period.
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© 1990 Kluwer Academic Publishers
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Kundt, W. (1990). Neutron-Star Accretion. In: Kundt, W. (eds) Neutron Stars and Their Birth Events. NATO ASI Series, vol 300. Springer, Dordrecht. https://doi.org/10.1007/978-94-009-0515-3_4
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DOI: https://doi.org/10.1007/978-94-009-0515-3_4
Publisher Name: Springer, Dordrecht
Print ISBN: 978-94-010-6718-8
Online ISBN: 978-94-009-0515-3
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