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Implications of magnetar non-precession

Implications of magnetar non-precession
Implications of magnetar non-precession
The objects known as anomalous X-ray pulsars and soft gamma repeaters are commonly identified with magnetars, neutron stars with ultrastrong magnetic fields. The rotational history of these objects has, so far, revealed no evidence of free precession. At the same time these objects do not generally appear to have magnetic axes nearly parallel or orthogonal to their spin axes. In this paper we show that the combination of these two observations, together with simple rigid-body dynamics, leads to non-trivial predictions about the interior properties of magnetars: either (i) elastic stresses in magnetar crusts are close to the theoretical upper limit above which the crustal matter yields or (ii) there is a "pinned" superfluid component in the magnetar interior. As a potentially observable consequence of these ideas we point out that, in the case of no pinned superfluidity, magnetars of stronger magnetic field strength than those currently observed would have to be nearly aligned/orthogonal rotators.
stars: magnetars, stars: neutron, stars: rotation
0035-8711
6
Glampedakis, K.
bece2036-f721-468e-9cd2-cf4324ff2deb
Jones, D.I.
b8f3e32c-d537-445a-a1e4-7436f472e160
Glampedakis, K.
bece2036-f721-468e-9cd2-cf4324ff2deb
Jones, D.I.
b8f3e32c-d537-445a-a1e4-7436f472e160

Glampedakis, K. and Jones, D.I. (2010) Implications of magnetar non-precession. Monthly Notices of the Royal Astronomical Society, 405, 6. (doi:10.1111/j.1745-3933.2010.00846.x).

Record type: Article

Abstract

The objects known as anomalous X-ray pulsars and soft gamma repeaters are commonly identified with magnetars, neutron stars with ultrastrong magnetic fields. The rotational history of these objects has, so far, revealed no evidence of free precession. At the same time these objects do not generally appear to have magnetic axes nearly parallel or orthogonal to their spin axes. In this paper we show that the combination of these two observations, together with simple rigid-body dynamics, leads to non-trivial predictions about the interior properties of magnetars: either (i) elastic stresses in magnetar crusts are close to the theoretical upper limit above which the crustal matter yields or (ii) there is a "pinned" superfluid component in the magnetar interior. As a potentially observable consequence of these ideas we point out that, in the case of no pinned superfluidity, magnetars of stronger magnetic field strength than those currently observed would have to be nearly aligned/orthogonal rotators.

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More information

Published date: 9 April 2010
Keywords: stars: magnetars, stars: neutron, stars: rotation

Identifiers

Local EPrints ID: 151807
URI: http://eprints.soton.ac.uk/id/eprint/151807
ISSN: 0035-8711
PURE UUID: bda71286-bd77-48fd-a60d-6ea419513565
ORCID for D.I. Jones: ORCID iD orcid.org/0000-0002-0117-7567

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Date deposited: 12 May 2010 14:19
Last modified: 09 Jan 2022 03:00

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Contributors

Author: K. Glampedakis
Author: D.I. Jones ORCID iD

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