Developing a model for neutron star oscillations following starquakes
Developing a model for neutron star oscillations following starquakes
Glitches – sudden increases in spin rate – are observed in many pulsars. One mechanism advanced to explain glitches in the youngest pulsars is that they are caused by a starquake, a sudden rearrangement of the crust of the neutron star. Starquakes have the potential to excite some of the oscillation modes of the neutron star, which means that they are of interest as a source of gravitational waves. These oscillations could also have an impact on radio emission. In this paper, we make upper estimates of the amplitude of the oscillations produced by a starquake, and the corresponding gravitational wave emission. We then develop a more detailed framework for calculating the oscillations excited by the starquake, using a toy model of a solid, incompressible star where all strain is lost instantaneously from the star at the glitch. For this toy model, we give plots of the amplitudes of the modes excited, as the shear modulus and rotation rate of the star are varied. We find that for our specific model, the largest excitation is generally of a mode similar to the f-mode of an incompressible fluid star, but that other modes of the star are excited to a significant degree over small parameter ranges of the rotation rate.
865-891
Keer, L.
27bbf851-bd12-40e4-acb4-f449e05ddb34
Jones, D.I.
b8f3e32c-d537-445a-a1e4-7436f472e160
January 2015
Keer, L.
27bbf851-bd12-40e4-acb4-f449e05ddb34
Jones, D.I.
b8f3e32c-d537-445a-a1e4-7436f472e160
Keer, L. and Jones, D.I.
(2015)
Developing a model for neutron star oscillations following starquakes.
Monthly Notices of the Royal Astronomical Society, 446 (1), .
(doi:10.1093/mnras/stu2123).
Abstract
Glitches – sudden increases in spin rate – are observed in many pulsars. One mechanism advanced to explain glitches in the youngest pulsars is that they are caused by a starquake, a sudden rearrangement of the crust of the neutron star. Starquakes have the potential to excite some of the oscillation modes of the neutron star, which means that they are of interest as a source of gravitational waves. These oscillations could also have an impact on radio emission. In this paper, we make upper estimates of the amplitude of the oscillations produced by a starquake, and the corresponding gravitational wave emission. We then develop a more detailed framework for calculating the oscillations excited by the starquake, using a toy model of a solid, incompressible star where all strain is lost instantaneously from the star at the glitch. For this toy model, we give plots of the amplitudes of the modes excited, as the shear modulus and rotation rate of the star are varied. We find that for our specific model, the largest excitation is generally of a mode similar to the f-mode of an incompressible fluid star, but that other modes of the star are excited to a significant degree over small parameter ranges of the rotation rate.
Text
865.full.pdf
- Version of Record
More information
Accepted/In Press date: 9 October 2014
e-pub ahead of print date: 13 November 2014
Published date: January 2015
Organisations:
Applied Mathematics
Identifiers
Local EPrints ID: 404332
URI: http://eprints.soton.ac.uk/id/eprint/404332
ISSN: 1365-2966
PURE UUID: 74a3d936-e5e7-4755-b648-3255f392ce64
Catalogue record
Date deposited: 05 Jan 2017 16:41
Last modified: 16 Mar 2024 03:06
Export record
Altmetrics
Contributors
Author:
L. Keer
Download statistics
Downloads from ePrints over the past year. Other digital versions may also be available to download e.g. from the publisher's website.
View more statistics
