Warping modes in discs around accreting neutron stars
H. Meheut, M. Tagger
TL;DR
This paper investigates the stability of plasma discs around accreting neutron stars, proposing a warping instability mechanism that could explain observed X-ray quasi-periodic oscillations.
Contribution
It introduces a new instability mechanism for magnetospheric discs, extending Pringle's radiation-driven warping model to neutron star systems.
Findings
Warping instability can reach high amplitudes
Mechanism may explain neutron star X-ray QPOs
Revises understanding of magnetospheric disc stability
Abstract
The origin and stability of a thin sheet of plasma in the magnetosphere of an accreting neutron star is investigated. First the radial extension of such a magnetospheric disc is explored. Then a mechanism for magnetospheric accretion is proposed, reconsidering the bending wave explored by Agapitou, Papaloizou & Terquem (1997), that was found to be stable in ideal MHD. We show that this warping becomes unstable and can reach high amplitudes, in a variant of Pringle's radiation-driven model for the warping of AGN accretion discs (Pringle (1996)). Finally we discuss how this mechanism might give a clue to explain the observed X-ray kHz QPO of neutron star binaries.
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