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Bumpy Spin-Down of Anomalous X-Ray Pulsars: The Link with Magnetars

Published online by Cambridge University Press:  12 April 2016

A. Melatos
A. Melatos*
Affiliation:
Department of Astronomy, 601 Campbell Hall, University of California at Berkeley, Berkeley CA 94720, USA

Abstract

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It is argued that bumps in the timing histories Ω(t) of the anomalous X-ray pulsars (AXPs) IE 1048.1-5937 and IE 2259+586 are the signature of a magnetar undergoing radiative precession, wherein the hydromagnetic deformation of the neutron star couples to an oscillating component of the vacuum-dipole radiation torque to produce an anharmonic wobble with period τpr ∼ 10 yr. An analysis of Euler’s equations of motion for a biaxial magnet reproduces the amplitude and recurrence time of the bumps for IE 1048.1-5937 and IE 2259+586, predicts Ω(t) for the next 20 years for both objects, and predicts a testable statistical relation between dΩ/dt and τpr for the AXP population overall. Radiative precession of soft gamma-ray repeaters is also discussed, together with implications for the internal (e.g. viscosity) and magnetospheric (e.g. e+e− pair currents) properties of magnetars.

Type
Part 10. Anomalous X-Ray Pulsars and Magnetars
Information
International Astronomical Union Colloquium , Volume 177: Pulsar Astronomy - 2000 and Beyond , 2000 , pp. 691 - 694
Copyright
Copyright © Astronomical Society of the Pacific 2000

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