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The flatness problem and Lambda.

Kayll Lake1

  • 1Department of Physics, Queen's University, Kingston, Ontario, Canada, K7L 3N6. lake@astro.queensu.ca

Physical Review Letters
|August 11, 2005
PubMed
Summary
This summary is machine-generated.

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The study reveals non-flat universe models with a positive cosmological constant (Lambda) where the density parameter (omega) stays near 1. Wilkinson Microwave Anisotropy Probe data supports these findings, indicating our universe is not finely tuned.

Area of Science:

  • Cosmology
  • General Relativity

Background:

  • The standard cosmological model assumes a flat universe.
  • The role of the cosmological constant (Lambda) in cosmic evolution is crucial.
  • Observational data, like the Wilkinson Microwave Anisotropy Probe (WMAP), provide constraints on cosmological parameters.

Purpose of the Study:

  • To investigate the existence and properties of non-flat Friedmann-Lemaître-Robertson-Walker (FLRW) models with a positive cosmological constant (Lambda).
  • To determine if these models require fine-tuning of cosmological parameters.
  • To assess the consistency of these models with observational data, particularly WMAP observations.

Main Methods:

  • Complete integration of the Friedmann equations in terms of observables.
  • Quantitative analysis of model parameter tuning.

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  • Comparison of theoretical predictions with observational data from WMAP.

    • Main Results:

    • Existence of non-flat FLRW models with Lambda > 0 where the total density parameter (omega) remains approximately 1 throughout cosmic history.
    • These models are shown to be not finely tuned in a precise quantitative sense.
    • WMAP observations confirm that our universe aligns with these specific non-flat models.

    Conclusions:

    • The universe can be non-flat and consistent with a positive cosmological constant (Lambda) without requiring fine-tuning.
    • Observational evidence, particularly from WMAP, supports the existence of such a universe.
    • The findings extend to models incorporating dark energy, reinforcing the viability of these non-flat, approximately critical density universes.