date: 2015-01-14T09:48:26Z
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pdf:docinfo:title: Quantum Gravity and Cosmological Density Perturbations
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subject: We explore the possible cosmological consequences of a running Newton's constant,  G ( ) , as suggested by the non-trivial ultraviolet fixed point scenario for Einstein gravity with a cosmological constant term. Here, we examine what possible effects a scale-dependent coupling might have on large-scale cosmological density perturbations. Starting from a set of manifestly covariant effective field equations, we develop the linear theory of density perturbations for a non-relativistic perfect fluid. The result is a modified equation for the matter density contrast, which can be solved and thus provides an estimate for the corrections to the growth index parameter, . 
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dc:title: Quantum Gravity and Cosmological Density Perturbations
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cp:subject: We explore the possible cosmological consequences of a running Newton's constant,  G ( ) , as suggested by the non-trivial ultraviolet fixed point scenario for Einstein gravity with a cosmological constant term. Here, we examine what possible effects a scale-dependent coupling might have on large-scale cosmological density perturbations. Starting from a set of manifestly covariant effective field equations, we develop the linear theory of density perturbations for a non-relativistic perfect fluid. The result is a modified equation for the matter density contrast, which can be solved and thus provides an estimate for the corrections to the growth index parameter, . 
pdf:docinfo:subject: We explore the possible cosmological consequences of a running Newton's constant,  G ( ) , as suggested by the non-trivial ultraviolet fixed point scenario for Einstein gravity with a cosmological constant term. Here, we examine what possible effects a scale-dependent coupling might have on large-scale cosmological density perturbations. Starting from a set of manifestly covariant effective field equations, we develop the linear theory of density perturbations for a non-relativistic perfect fluid. The result is a modified equation for the matter density contrast, which can be solved and thus provides an estimate for the corrections to the growth index parameter, . 
pdf:docinfo:creator: Herbert W. Hamber, Reiko Toriumi
meta:author: Herbert W. Hamber, Reiko Toriumi
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dc:description: We explore the possible cosmological consequences of a running Newton's constant,  G ( ) , as suggested by the non-trivial ultraviolet fixed point scenario for Einstein gravity with a cosmological constant term. Here, we examine what possible effects a scale-dependent coupling might have on large-scale cosmological density perturbations. Starting from a set of manifestly covariant effective field equations, we develop the linear theory of density perturbations for a non-relativistic perfect fluid. The result is a modified equation for the matter density contrast, which can be solved and thus provides an estimate for the corrections to the growth index parameter, . 
Keywords: "quantum gravity; quantum cosmology; renormalization group; quantum infrared effects"
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dc:creator: Herbert W. Hamber, Reiko Toriumi
description: We explore the possible cosmological consequences of a running Newton's constant,  G ( ) , as suggested by the non-trivial ultraviolet fixed point scenario for Einstein gravity with a cosmological constant term. Here, we examine what possible effects a scale-dependent coupling might have on large-scale cosmological density perturbations. Starting from a set of manifestly covariant effective field equations, we develop the linear theory of density perturbations for a non-relativistic perfect fluid. The result is a modified equation for the matter density contrast, which can be solved and thus provides an estimate for the corrections to the growth index parameter, . 
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title: Quantum Gravity and Cosmological Density Perturbations
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dc:subject: "quantum gravity; quantum cosmology; renormalization group; quantum infrared effects"
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