2014
DOI: 10.1142/s0218271814500175
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Perturbation of FRW Spacetime in Np Formalism

Abstract: Jacobi polynomials appear to play a very important role in describing all the spin field (s = 0, 1/2, 1, 2) perturbation of the FRW spacetime. The formulation becomes very transparent when done in NP formalism. All the variables are separable, and the spatial eigenfuctions turn out to be Jacobian polynomials in different forms. In particular, the angular ones are expressible as spin weighted spherical harmonics which are just the spherical harmonics formed with Jacobi polynomials. The radial eigenfuctions are … Show more

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Cited by 6 publications
(2 citation statements)
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“…Progress in perturbation analysis in FLRW spacetime is essential for advancing our understanding of the universe's large-scale structure and testing fundamental theories of cosmology and gravity. That's why the perturbations in FLRW spacetime have been further investigated in this paper extending authors' previous work 11 In terms of Jacobi polynomials 14 , 𝑃 𝑛 (𝛼,𝛽) , the angular and spatial parts are given respectively as…”
Section: Introductionsupporting
confidence: 62%
“…Progress in perturbation analysis in FLRW spacetime is essential for advancing our understanding of the universe's large-scale structure and testing fundamental theories of cosmology and gravity. That's why the perturbations in FLRW spacetime have been further investigated in this paper extending authors' previous work 11 In terms of Jacobi polynomials 14 , 𝑃 𝑛 (𝛼,𝛽) , the angular and spatial parts are given respectively as…”
Section: Introductionsupporting
confidence: 62%
“…In this work, we investigate the behaviour of the massive Klein-Gordon (KG) 1, 2 field coupled to the Friedman-Lemaitre-Robertson-Walker (FLRW) background geometry. In our previous work 3 , we were able to write down and solve the equations governing the perturbation of FLRW space-time in Neumann-Penrose formalism 4,5 . The angular eigen functions turn out to be the spinweighted spherical harmonics p Y m l of weight p=0, ±1,±2, corresponding to scalar, vectorial and tensorial perturbations.…”
Section: Introductionmentioning
confidence: 99%