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<p>The density perturbations of the universe have been considered in the framework of a Finslerian cosmological model, in which the background spacetime of the universe is taken as the spatially flat FLRW spacetime with a Finslerian perturbation. The inhomogeneity in the matter (energy) density arises naturally in this consideration of gravity in the <InlineEquation ID="IEq1"> <EquationSource Format="TEX">\((\alpha , \beta )\)</EquationSource> <EquationSource Format="MATHML"><math> <mrow> <mo stretchy="false">(</mo> <mi>α</mi> <mo>,</mo> <mi>β</mi> <mo stretchy="false">)</mo> </mrow> </math></EquationSource> </InlineEquation>-Finsler space for the background spacetime of the universe. The resulting inhomogeneous matter density indicates matter perturbation departing from the uniform density, and it is caused by the Finslerian perturbation in the Riemannian spacetime, thus ascertaining the geometrical origin of the growth of matter perturbations.</p>

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Geometrical origin of growth of matter perturbations in Finslerian background

  • 期刊论文

  • 发表日期：

    2026年3月25日

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  • S. S. De,
  • Farook Rahaman,
  • Antara Mapdar

摘要

The density perturbations of the universe have been considered in the framework of a Finslerian cosmological model, in which the background spacetime of the universe is taken as the spatially flat FLRW spacetime with a Finslerian perturbation. The inhomogeneity in the matter (energy) density arises naturally in this consideration of gravity in the \((\alpha , \beta )\) ( α , β ) -Finsler space for the background spacetime of the universe. The resulting inhomogeneous matter density indicates matter perturbation departing from the uniform density, and it is caused by the Finslerian perturbation in the Riemannian spacetime, thus ascertaining the geometrical origin of the growth of matter perturbations.