Modelling magnetically deformed neutron stars
Modelling magnetically deformed neutron stars
Rotating deformed neutron stars are important potential sources for ground-based gravitational wave interferometers such as LIGO, GEO600 and VIRGO. One mechanism that may lead to significant non-asymmetries is the internal magnetic field. It is well known that a magnetic star will not be spherical and, if the magnetic axis is not aligned with the spin axis, the deformation will lead to the emission of gravitational waves. The aim of this paper is to develop a formalism that would allow us to model magnetically deformed stars, using both realistic equations of state and field configurations. As a first step, we consider a set of simplified model problems. Focusing on dipolar fields, we determine the internal magnetic field which is consistent with a given neutron star model and calculate the associated deformation. We discuss the relevance of our results for current gravitational wave detectors and future prospects.
531-542
Haskell, B.
a3c09067-6932-45cc-902d-3b7117ec848d
Samuelsson, L.
972a981e-08d5-4c5e-a462-fa36c0af9faa
Glampedakis, K.
bece2036-f721-468e-9cd2-cf4324ff2deb
Andersson, N.
2dd6d1ee-cefd-478a-b1ac-e6feedafe304
March 2008
Haskell, B.
a3c09067-6932-45cc-902d-3b7117ec848d
Samuelsson, L.
972a981e-08d5-4c5e-a462-fa36c0af9faa
Glampedakis, K.
bece2036-f721-468e-9cd2-cf4324ff2deb
Andersson, N.
2dd6d1ee-cefd-478a-b1ac-e6feedafe304
Haskell, B., Samuelsson, L., Glampedakis, K. and Andersson, N.
(2008)
Modelling magnetically deformed neutron stars.
Monthly Notices of the Royal Astronomical Society, 385 (1), .
(doi:10.1111/j.1365-2966.2008.12861.x).
Abstract
Rotating deformed neutron stars are important potential sources for ground-based gravitational wave interferometers such as LIGO, GEO600 and VIRGO. One mechanism that may lead to significant non-asymmetries is the internal magnetic field. It is well known that a magnetic star will not be spherical and, if the magnetic axis is not aligned with the spin axis, the deformation will lead to the emission of gravitational waves. The aim of this paper is to develop a formalism that would allow us to model magnetically deformed stars, using both realistic equations of state and field configurations. As a first step, we consider a set of simplified model problems. Focusing on dipolar fields, we determine the internal magnetic field which is consistent with a given neutron star model and calculate the associated deformation. We discuss the relevance of our results for current gravitational wave detectors and future prospects.
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Published date: March 2008
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Local EPrints ID: 54976
URI: http://eprints.soton.ac.uk/id/eprint/54976
ISSN: 1365-2966
PURE UUID: 29884158-a126-497f-9da1-f6e113087826
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Date deposited: 04 Aug 2008
Last modified: 16 Mar 2024 03:02
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Author:
B. Haskell
Author:
L. Samuelsson
Author:
K. Glampedakis
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