Oscillations of general relativistic multi-fluid/multi-layer compact star
Oscillations of general relativistic multi-fluid/multi-layer compact star
We develop the formalism for determining the quasinormal modes of general relativistic multifluid
compact stars in such a way that the impact of superfluid gap data can be assessed. Our
results represent the first attempt to study true multi-layer dynamics, an important step towards
considering realistic superfluid/superconducting compact stars. We combine a relativistic model
for entrainment with model equations of state that explicity incorporate the symmetry energy. Our
analysis emphasises the many different parameters that are required for this kind of modelling, and
the fact that standard tabulated equations of state are grossly incomplete in this respect. To make
progress, future equations of state need to provide the energy density as a function of the various
nucleon number densities, the temperature (i.e. entropy), and the entrainment among the various
components.
Lin, L.
81b0bec5-350e-471b-b372-cfe220b824b3
Andersson, N.
2dd6d1ee-cefd-478a-b1ac-e6feedafe304
Comer, G.L
0ee3a15e-e5c6-43f8-9903-d76faa820bd9
Lin, L.
81b0bec5-350e-471b-b372-cfe220b824b3
Andersson, N.
2dd6d1ee-cefd-478a-b1ac-e6feedafe304
Comer, G.L
0ee3a15e-e5c6-43f8-9903-d76faa820bd9
Lin, L., Andersson, N. and Comer, G.L
(2007)
Oscillations of general relativistic multi-fluid/multi-layer compact star.
Pre-print.
(Submitted)
Abstract
We develop the formalism for determining the quasinormal modes of general relativistic multifluid
compact stars in such a way that the impact of superfluid gap data can be assessed. Our
results represent the first attempt to study true multi-layer dynamics, an important step towards
considering realistic superfluid/superconducting compact stars. We combine a relativistic model
for entrainment with model equations of state that explicity incorporate the symmetry energy. Our
analysis emphasises the many different parameters that are required for this kind of modelling, and
the fact that standard tabulated equations of state are grossly incomplete in this respect. To make
progress, future equations of state need to provide the energy density as a function of the various
nucleon number densities, the temperature (i.e. entropy), and the entrainment among the various
components.
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Submitted date: September 2007
Additional Information:
2007arXiv0709.0660L
Identifiers
Local EPrints ID: 54970
URI: http://eprints.soton.ac.uk/id/eprint/54970
PURE UUID: 527ee18c-15a2-48ae-94ff-c5b769fe0be9
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Date deposited: 01 Aug 2008
Last modified: 12 Dec 2021 03:04
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Contributors
Author:
L. Lin
Author:
G.L Comer
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