A hydrodynamical trigger mechanism for pulsar glitches
A hydrodynamical trigger mechanism for pulsar glitches
The standard explanation for large pulsar glitches involves transfer of angular momentum from an internal superfluid component to the star's crust. This model requires an instability to trigger the sudden unpinning of the vortices by means of which the superfluid rotates. This Letter describes a new instability that may play this role. The instability, which is associated with the inertial r-modes of a superfluid neutron star, sets in once the rotational lag in the system reaches a critical level. We demonstrate that our model is in good agreement with observed glitch data, suggesting that the superfluid r-mode instability may indeed be the mechanism that triggers large pulsar glitches.
5pp
Glampedakis, K.
bece2036-f721-468e-9cd2-cf4324ff2deb
Andersson, N.
2dd6d1ee-cefd-478a-b1ac-e6feedafe304
Glampedakis, K.
bece2036-f721-468e-9cd2-cf4324ff2deb
Andersson, N.
2dd6d1ee-cefd-478a-b1ac-e6feedafe304
Abstract
The standard explanation for large pulsar glitches involves transfer of angular momentum from an internal superfluid component to the star's crust. This model requires an instability to trigger the sudden unpinning of the vortices by means of which the superfluid rotates. This Letter describes a new instability that may play this role. The instability, which is associated with the inertial r-modes of a superfluid neutron star, sets in once the rotational lag in the system reaches a critical level. We demonstrate that our model is in good agreement with observed glitch data, suggesting that the superfluid r-mode instability may indeed be the mechanism that triggers large pulsar glitches.
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Submitted date: 23 June 2008
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arXiv:0806.3664v1
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Applied Mathematics
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Local EPrints ID: 54977
URI: http://eprints.soton.ac.uk/id/eprint/54977
PURE UUID: 3086b39f-7c81-4ed1-806a-ef0edc3c8f88
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Date deposited: 04 Aug 2008
Last modified: 16 Mar 2024 03:02
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Author:
K. Glampedakis
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