Seismology of adolescent neutron stars: Accounting for thermal effects and crust elasticity
Seismology of adolescent neutron stars: Accounting for thermal effects and crust elasticity
We study the oscillations of relativistic stars, incorporating key physics associated with internal composition, thermal gradients and crust elasticity. Our aim is to develop a formalism which is able to account for the state-of-the-art understanding of the complex physics associated with these systems. As a first step, we build models using a modern equation of state including composition gradients and density discontinuities associated with internal phase transitions (like the crust-core transition and the point where muons first appear in the core). In order to understand the nature of the oscillation spectrum, we carry out cooling simulations to provide realistic snapshots of the temperature distribution in the interior as the star evolves through adolescence. The associated thermal pressure is incorporated in the perturbation analysis, and we discuss the presence of g-modes arising as a result of thermal effects. We also consider interface modes due to phase-transitions and the gradual formation of the star's crust and the emergence of a set of shear modes.
063009-[22pp]
Krueger, Christian J.
9468e292-0b41-412d-9470-944e257c7bcf
Ho, Wynn C.G.
d78d4c52-8f92-4846-876f-e04a8f803a45
Andersson, Nils
2dd6d1ee-cefd-478a-b1ac-e6feedafe304
10 September 2015
Krueger, Christian J.
9468e292-0b41-412d-9470-944e257c7bcf
Ho, Wynn C.G.
d78d4c52-8f92-4846-876f-e04a8f803a45
Andersson, Nils
2dd6d1ee-cefd-478a-b1ac-e6feedafe304
Krueger, Christian J., Ho, Wynn C.G. and Andersson, Nils
(2015)
Seismology of adolescent neutron stars: Accounting for thermal effects and crust elasticity.
Physical Review D, 92 (6), .
(doi:10.1103/PhysRevD.92.063009).
Abstract
We study the oscillations of relativistic stars, incorporating key physics associated with internal composition, thermal gradients and crust elasticity. Our aim is to develop a formalism which is able to account for the state-of-the-art understanding of the complex physics associated with these systems. As a first step, we build models using a modern equation of state including composition gradients and density discontinuities associated with internal phase transitions (like the crust-core transition and the point where muons first appear in the core). In order to understand the nature of the oscillation spectrum, we carry out cooling simulations to provide realistic snapshots of the temperature distribution in the interior as the star evolves through adolescence. The associated thermal pressure is incorporated in the perturbation analysis, and we discuss the presence of g-modes arising as a result of thermal effects. We also consider interface modes due to phase-transitions and the gradual formation of the star's crust and the emergence of a set of shear modes.
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Published date: 10 September 2015
Organisations:
Applied Mathematics
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Local EPrints ID: 379901
URI: http://eprints.soton.ac.uk/id/eprint/379901
ISSN: 1550-7998
PURE UUID: 0fca1403-96cd-4b94-bc8a-655bec7c747a
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Date deposited: 24 Aug 2015 13:04
Last modified: 15 Mar 2024 02:59
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Author:
Christian J. Krueger
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