r-modes in low temperature color-flavor-locked superconducting quark stars
r-modes in low temperature color-flavor-locked superconducting quark stars
We present the first multifluid analysis of a dense neutron star core with a deconfined color-flavor-locked superconducting quark component. Accounting only for the condensate and (finite temperature) phonons, we make progress by taking over results for superfluid 4He. The resultant two-fluid model accounts for a number of additional viscosity coefficients (compared to the Navier-Stokes equations) and we show how they enter the dissipation analysis for an oscillating star. We provide simple estimates for the gravitational-wave driven r-mode instability, demonstrating that the various phonon processes that we consider are not effective damping agents. Even though the results are likely of little direct astrophysical importance (since we consider an overly simplistic stellar model) our analysis represents significant technical progress, laying the foundation for more detailed numerical studies and preparing the ground for the inclusion of additional aspects (in particular associated with kaons) of the problem
023007-[15]
Andersson, Nils
2dd6d1ee-cefd-478a-b1ac-e6feedafe304
Haskell, B.
a3c09067-6932-45cc-902d-3b7117ec848d
Comer, G.L.
f2c1746c-8638-4268-94f0-e5d4375f0358
July 2010
Andersson, Nils
2dd6d1ee-cefd-478a-b1ac-e6feedafe304
Haskell, B.
a3c09067-6932-45cc-902d-3b7117ec848d
Comer, G.L.
f2c1746c-8638-4268-94f0-e5d4375f0358
Andersson, Nils, Haskell, B. and Comer, G.L.
(2010)
r-modes in low temperature color-flavor-locked superconducting quark stars.
Physical Review D, 82 (2), .
(doi:10.1103/PhysRevD.82.023007).
Abstract
We present the first multifluid analysis of a dense neutron star core with a deconfined color-flavor-locked superconducting quark component. Accounting only for the condensate and (finite temperature) phonons, we make progress by taking over results for superfluid 4He. The resultant two-fluid model accounts for a number of additional viscosity coefficients (compared to the Navier-Stokes equations) and we show how they enter the dissipation analysis for an oscillating star. We provide simple estimates for the gravitational-wave driven r-mode instability, demonstrating that the various phonon processes that we consider are not effective damping agents. Even though the results are likely of little direct astrophysical importance (since we consider an overly simplistic stellar model) our analysis represents significant technical progress, laying the foundation for more detailed numerical studies and preparing the ground for the inclusion of additional aspects (in particular associated with kaons) of the problem
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Published date: July 2010
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Local EPrints ID: 181251
URI: http://eprints.soton.ac.uk/id/eprint/181251
ISSN: 2470-0029
PURE UUID: 988e0e3b-cdb8-45ff-85f5-5c9b65fd11c5
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Date deposited: 15 Apr 2011 13:47
Last modified: 15 Mar 2024 02:59
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Author:
B. Haskell
Author:
G.L. Comer
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