The dynamics of pulsar glitches: contrasting phenomenology with numerical evolutions
The dynamics of pulsar glitches: contrasting phenomenology with numerical evolutions
In this paper, we consider a simple two-fluid model for pulsar glitches. We derive the basic equations that govern the spin evolution of the system from two-fluid hydrodynamics, accounting for the vortex mediated mutual friction force that determines the glitch rise. This leads to a simple 'bulk' model that can be used to describe the main properties of a glitch event resulting from vortex unpinning.
In order to model the long-term relaxation following the glitch, our model would require additional assumptions regarding the repinning of vortices, an issue that we only touch upon briefly. Instead, we focus on comparing the phenomenological model to results obtained from time-evolutions of the linearized two-fluid equations, i.e. a 'hydrodynamic' model for glitches. This allows us to study, for the first time, dynamics that was 'averaged' in the bulk model, i.e. consider the various neutron star oscillation modes that are excited during a glitch.
The hydro-results are of some relevance for efforts to detect gravitational waves from glitching pulsars, although the conclusions drawn from our rather simple model are pessimistic as far as the detectability of these events is concerned.
gravitational waves, methods: numerical, stars: neutron, stars: oscillations, pulsars: general
Sidery, T.
bc971e4a-89f6-4e64-aa6e-9fefac007786
Passamonti, A.
d9c7544a-5b0e-4230-9caa-f5a9a6fe9f13
Andersson, N.
2dd6d1ee-cefd-478a-b1ac-e6feedafe304
14 April 2010
Sidery, T.
bc971e4a-89f6-4e64-aa6e-9fefac007786
Passamonti, A.
d9c7544a-5b0e-4230-9caa-f5a9a6fe9f13
Andersson, N.
2dd6d1ee-cefd-478a-b1ac-e6feedafe304
Sidery, T., Passamonti, A. and Andersson, N.
(2010)
The dynamics of pulsar glitches: contrasting phenomenology with numerical evolutions.
Monthly Notices of the Royal Astronomical Society.
(doi:10.1111/j.1365-2966.2010.16497.x).
Abstract
In this paper, we consider a simple two-fluid model for pulsar glitches. We derive the basic equations that govern the spin evolution of the system from two-fluid hydrodynamics, accounting for the vortex mediated mutual friction force that determines the glitch rise. This leads to a simple 'bulk' model that can be used to describe the main properties of a glitch event resulting from vortex unpinning.
In order to model the long-term relaxation following the glitch, our model would require additional assumptions regarding the repinning of vortices, an issue that we only touch upon briefly. Instead, we focus on comparing the phenomenological model to results obtained from time-evolutions of the linearized two-fluid equations, i.e. a 'hydrodynamic' model for glitches. This allows us to study, for the first time, dynamics that was 'averaged' in the bulk model, i.e. consider the various neutron star oscillation modes that are excited during a glitch.
The hydro-results are of some relevance for efforts to detect gravitational waves from glitching pulsars, although the conclusions drawn from our rather simple model are pessimistic as far as the detectability of these events is concerned.
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Published date: 14 April 2010
Keywords:
gravitational waves, methods: numerical, stars: neutron, stars: oscillations, pulsars: general
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Local EPrints ID: 151319
URI: http://eprints.soton.ac.uk/id/eprint/151319
ISSN: 1365-2966
PURE UUID: 54ae9b46-c383-42fa-b630-fceaa75ab8a6
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Date deposited: 10 May 2010 11:00
Last modified: 14 Mar 2024 02:42
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Author:
T. Sidery
Author:
A. Passamonti
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