Burial of the polar magnetic field of an accreting neutron star – II. Hydromagnetic stability of axisymmetric equilibria

• Published in: Monthly notices of the Royal Astronomical Society 2007-04, Vol.376 (2), p.609-624
• Main Authors: Payne, D. J. B., Melatos, A.
• Format: Article
• Language: English
• Subjects: accretion; accretion discs; accretion, accretion discs; Astronomy; Astrophysics; Earth, ocean, space; Exact sciences and technology; Magnetic fields; Mathematical models; pulsars: general; Stars & galaxies; stars: magnetic fields; stars: neutron
• ISSN: 0035-8711; 1365-2966
• DOI: 10.1111/j.1365-2966.2007.11451.x

The theory of polar magnetic burial in accreting neutron stars predicts that a mountain of accreted material accumulates at the magnetic poles of the star, and that, as the mountain spreads equatorward, it is confined by, and compresses, the equatorial magnetic field. Here, we extend previous, axisymmetric, Grad–Shafranov calculations of the hydromagnetic structure of a magnetic mountain up to accreted masses as high as Ma= 6 × 10−4 M⊙, by importing the output from previous calculations (which were limited by numerical problems and the formation of closed bubbles to Ma < 10−4 M⊙) into the time-dependent, ideal-magnetohydrodynamic code zeus-3d and loading additional mass on to the star dynamically. The rise of buoyant magnetic bubbles through the accreted layer is observed in these experiments. We also investigate the stability of the resulting hydromagnetic equilibria by perturbing them in zeus-3d. Surprisingly, it is observed that the equilibria are marginally stable for all Ma≤ 6 × 10−4 M⊙; the mountain oscillates persistently when perturbed, in a combination of Alfvén and acoustic modes, without appreciable damping or growth, and is therefore not disrupted (apart from a transient Parker instability initially, which expels