Self-gravitating static balls of power-law elastic matter

Alho, Artur; Calogero, Simone; Liljenberg, Astrid

doi:10.48550/arxiv.2104.11131

Cited by 2 publications

(2 citation statements)

References 11 publications

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“…Here s can be interpreted as the shear index; when s ¼ n and ε ¼ 0 we recover the usual relativistic polytropes (see also [34,35] for similar stored energy functions in the Newtonian setting). The Lamé parameters are the same as in the quadratic model (12), and in fact the two models coincide when s ¼ n ¼ 1.…”

Section: Materials Modelsmentioning

confidence: 85%

Compact elastic objects in general relativity

et al. 2022

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We introduce a rigorous and general framework to study systematically self-gravitating elastic materials within general relativity, and apply it to investigate the existence and viability, including radial stability, of spherically symmetric elastic stars. We present the mass-radius (M − R) diagram for various families of models, showing that elasticity contributes to increasing the maximum mass and the compactness up to ≈22%, thus supporting compact stars with mass well above two solar masses. Some of these elastic stars can reach compactness as high as GM=ðc 2 RÞ ≈ 0.35 while remaining stable under radial perturbations and satisfying all energy conditions and subluminal wave propagation, thus being physically realizable models of stars with a light ring. We provide numerical evidence that radial instability occurs for central densities larger than that corresponding to the maximum mass, as in the perfect-fluid case. Elasticity may be a key ingredient to building consistent models of exotic ultracompact objects and black hole mimickers, and can also be relevant for a more accurate modeling of the interior of neutron stars.

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Section: Materials Modelsmentioning

confidence: 85%

Compact elastic objects in general relativity

et al. 2022

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“…Here s can be interpreted as the shear index; when s = n and ε = 0 we recover the usual relativistic polytropes. This function w(δ, η) is similar to the power-law stored energy function (2.18) in [33], which belongs to a more general class of polytropic elastic materials introduced (11) with n = 1/2 and K = 6 × 10 4 M 4 (left) and for the two-parameter elastic model (12) with n = 1 and K = 100M 2 (right). Solid (dashed) curves correspond to configurations with subluminal (superluminal) wave propagation.…”

Section: Introductionmentioning

confidence: 93%

Compact elastic objects in general relativity

Alho,

Natário,

Pani

et al. 2021

Preprint

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We introduce a rigorous and general framework to study systematically self-gravitating elastic materials within general relativity, and apply it to investigate the existence and viability, including radial stability, of spherically symmetric elastic stars. We present the mass-radius (M − R) diagram for various families of models, showing that elasticity contributes to increase the maximum mass and the compactness up to a O(10%) factor, thus supporting compact stars with mass well above two solar masses. Some of these elastic stars can reach compactness as high as GM/(c 2 R) ≈ 0.35 while remaining stable under radial perturbations and satisfying all energy conditions and subluminal wave propagation, thus being physically viable models of stars with a light ring. We provide numerical evidence that radial instability occurs for central densities larger than that corresponding to the maximum mass, as in the perfect-fluid case. Elasticity may be a key ingredient to build consistent models of exotic ultracompact objects and black-hole mimickers, and can also be relevant for a more accurate modelling of the interior of neutron stars.

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Self-gravitating static balls of power-law elastic matter

Cited by 2 publications

References 11 publications

Compact elastic objects in general relativity

Compact elastic objects in general relativity

Compact elastic objects in general relativity

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